Ultracold atomic gases is a rapidly developing area of physics that attracts many young researchers around the world. Wr

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T.C. Choy: Eﬀective medium theory, Second edition L. Pitaevskii, S. Stringari: Bose–Einstein condensation and superﬂuidity B.J. Dalton, J. Jeﬀers, S.M. Barnett: Phase space methods for degenerate quantum gases W.D. McComb: Homogeneous, isotropic turbulence – phenomenology, renormalization and statistical closures V.Z. Kresin, H. Morawitz, S.A. Wolf: Superconducting state – mechanisms and properties C. Barrab` es, P.A. Hogan: Advanced general relativity – gravity waves, spinning particles, and black holes W. Barford: Electronic and optical properties of conjugated polymers, Second edition F. Strocchi: An introduction to non-perturbative foundations of quantum ﬁeld theory K.H. Bennemann, J.B. Ketterson: Novel superﬂuids, Volume 2 K.H. Bennemann, J.B. Ketterson: Novel superﬂuids, Volume 1 C. Kiefer: Quantum gravity, Third edition L. Mestel: Stellar magnetism, Second edition R.A. Klemm: Layered superconductors, Volume 1 E.L. Wolf: Principles of electron tunneling spectroscopy, Second edition R. Blinc: Advanced ferroelectricity L. Berthier, G. Biroli, J.-P. Bouchaud, W. van Saarloos, L. Cipelletti: Dynamical heterogeneities in glasses, colloids, and granular media J. Wesson: Tokamaks, Fourth edition H. Asada, T. Futamase, P. Hogan: Equations of motion in general relativity A. Yaouanc, P. Dalmas de R´ eotier: Muon spin rotation, relaxation, and resonance B. McCoy: Advanced statistical mechanics M. Bordag, G.L. Klimchitskaya, U. Mohideen, V.M. Mostepanenko: Advances in the Casimir eﬀect T.R. Field: Electromagnetic scattering from random media W. G¨ otze: Complex dynamics of glass-forming liquids – a mode-coupling theory V.M. Agranovich: Excitations in organic solids W.T. Grandy: Entropy and the time evolution of macroscopic systems M. Alcubierre: Introduction to 3 + 1 numerical relativity A.L. Ivanov, S.G. Tikhodeev: Problems of condensed matter physics – quantum coherence phenomena in electron-hole and coupled matter-light systems I.M. Vardavas, F.W. Taylor: Radiation and climate A.F. Borghesani: Ions and electrons in liquid helium V. Fortov, I. Iakubov, A. Khrapak: Physics of strongly coupled plasma G. Fredrickson: The equilibrium theory of inhomogeneous polymers H. Suhl: Relaxation processes in micromagnetics J. Terning: Modern supersymmetry M. Mari˜ no: Chern-Simons theory, matrix models, and topological strings V. Gantmakher: Electrons and disorder in solids W. Barford: Electronic and optical properties of conjugated polymers R.E. Raab, O.L. de Lange: Multipole theory in electromagnetism A. Larkin, A. Varlamov: Theory of ﬂuctuations in superconductors P. Goldbart, N. Goldenfeld, D. Sherrington: Stealing the gold S. Atzeni, J. Meyer-ter-Vehn: The physics of inertial fusion T. Fujimoto: Plasma spectroscopy K. Fujikawa, H. Suzuki: Path integrals and quantum anomalies T. Giamarchi: Quantum physics in one dimension M. Warner, E. Terentjev: Liquid crystal elastomers L. Jacak, P. Sitko, K. Wieczorek, A. Wojs: Quantum Hall systems G. Volovik: The Universe in a helium droplet L. Pitaevskii, S. Stringari: Bose–Einstein condensation G. Dissertori, I.G. Knowles, M. Schmelling: Quantum chromodynamics B. DeWitt: The global approach to quantum ﬁeld theory J. Zinn-Justin: Quantum ﬁeld theory and critical phenomena, Fourth edition R.M. Mazo: Brownian motion – ﬂuctuations, dynamics, and applications H. Nishimori: Statistical physics of spin glasses and information processing – an introduction N.B. Kopnin: Theory of nonequilibrium superconductivity A. Aharoni: Introduction to the theory of ferromagnetism, Second edition R. Dobbs: Helium three R. Wigmans: Calorimetry J. K¨ ubler: Theory of itinerant electron magnetism Y. Kuramoto, Y. Kitaoka: Dynamics of heavy electrons D. Bardin, G. Passarino: The Standard Model in the making G.C. Branco, L. Lavoura, J.P. Silva: CP Violation T.C. Choy: Eﬀective medium theory H. Araki: Mathematical theory of quantum ﬁelds L.M. Pismen: Vortices in nonlinear ﬁelds

Bose–Einstein Condensation and Superfluidity Lev Pitaevskii Department of Physics, University of Trento and National Institute of Optics, INO-CNR, Italy Kapitza Institute for Physical Problems, RAS, Moscow, Russia

Sandro Stringari Department of Physics, University of Trento and National Institute of Optics, INO-CNR, Italy

3

3

Great Clarendon Street, Oxford, OX2 6DP, United Kingdom Oxford University Press is a department of the University of Oxford. It furthers the University’s objective of excellence in research, scholarship, and education by publishing worldwide. Oxford is a registered trade mark of Oxford University Press in the UK and in certain other countries c Lev Pitaevskii and Sandro Stringari 2016 The moral rights of the authors have been asserted First Edition published in 2016 Impression: 1 All rights reserved. No part of this publication may be reproduced, stored in a retrieval system, or transmitted, in any form or by any means, without the prior permission in writing of Oxford University Press, or as expressly permitted by law, by licence or under terms agreed with the appropriate reprographics rights organization. Enquiries concerning reproduction outside the scope of the above should be sent to the Rights Department, Oxford University Press, at the address above You must not circulate this work in any other form and you must impose this same condition on any acquirer Published in the United States of America by Oxford University Press 198 Madison Avenue, New York, NY 10016, United States of America British Library Cataloguing in Publication Data Data available Library of Congress Control Number: 2015947456 ISBN 978–0–19–875888–4 Printed and bound by CPI Group (UK) Ltd, Croydon, CR0 4YY

Preface This is an extended and updated version of the book Bose–Einstein Condensation, published by Oxford University Press in 2003. Its writing was stimulated by continuous and exciting developments in the ﬁeld of ultracold atoms, which started after the ﬁrst experimental realization of Bose–Einstein Condensation (BEC) in atomic gases, achieved in 1995, and are still involving several hundreds of scientists around the world. While the basic theory of BEC had been developed before 1995, its application to the new conﬁgurations realized with magnetic and optical trapping is more recent and has revealed numerous unexpected features, stimulating further experimental and theoretical work. In the ﬁrst part of this volume we focus on the key theoretical concepts underlying the physics of Bose–Einstein condensation, in connection with the fundamental developments in the theory which took place before 1995. In the second part the main emphasis is instead given to the consequences of BEC on atomic Bose gases cooled and conﬁned in traps. These systems are highly inhomogeneous and consequently exhibit novel features which are presently the object of intense research activity. The third part of the volume deals with the physics of ultracold Fermi gases, whose experimental investigation has shown a terriﬁc development in the last ten years, giving a new insight in many problems of condensed matter physics with deep connections with the physics of Bose–Einstein condensation and superﬂuidity. The last part covers topics of joint interest for the study of Bose and Fermi gases, like the new phenomena exhibited in optical traps and in low dimensional conﬁgurations, the properties of quantum mixtures, and the consequences of long-range dipolar interactions. In writing this book we have proﬁted from stimulating discussions and collaborations with many colleagues around the world. It is a special pleasure to thank the friends of the Trento group and, in particular, Iacopo Carusotto, Franco Dalfovo, Gabriele Ferrari, Stefano Giorgini, Giacomo Lamporesi, Chiara Menotti, and Alessio Recati. We are also grateful to Giovanni Martone for his help in the ﬁnal preparation of the book. Trento July, 2015

L.P. S.S.

Contents 1

Introduction

1

PART I 2

Long-range Order, Symmetry Breaking, and Order Parameter 2.1 One-body density matrix and long-range order 2.2 Order parameter

9 9 13

3

The 3.1 3.2 3.3

15 15 19 26

4

Weakly Interacting Bose Gas 4.1 Lowest-order approximation: ground state energy and equation of state 4.2 Higher-order approximation: excitation spectrum and quantum ﬂuctuations 4.3 Particles and elementary excitations

Ideal Bose Gas The ideal Bose gas in the grand canonical ensemble The ideal Bose gas in the box Fluctuations and two-body density

29 29 33 37

5

Nonuniform Bose Gases at Zero Temperature 5.1 The Gross–Pitaevskii equation 5.2 Thomas–Fermi limit 5.3 Vortex line in the weakly interacting Bose gas 5.4 Vortex rings 5.5 Solitons 5.6 Small-amplitude oscillations

42 42 47 48 51 55 60

6

Superﬂuidity 6.1 Landau’s criterion of superﬂuidity 6.2 Bose–Einstein condensation and superﬂuidity 6.3 Hydrodynamic theory of superﬂuids: zero temperature 6.4 Quantum hydrodynamics 6.5 Beliaev decay of phonons 6.6 Two-ﬂuid hydrodynamics: ﬁrst and second sound 6.7 Fluctuations of the phase 6.8 Rotation of superﬂuids

65 65 69 70 71 74 76 81 85

7

Linear Response Function 7.1 Dynamic structure factor and sum rules 7.2 Density response function

89 89 94

viii

Contents

7.3 7.4 7.5 7.6

Current response function General inequalities Response function of the ideal Bose gas Response function of the weakly interacting Bose gas

98 100 105 107

8

Superﬂuid 4 He 8.1 Elementary excitations and dynamic structure factor 8.2 Thermodynamic properties 8.3 Quantized vortices 8.4 Momentum distribution and Bose–Einstein condensation

110 110 118 121 125

9

Atomic Gases: Collisions and Trapping 9.1 Metastability and the role of collisions 9.2 Low-energy collisions and scattering length 9.3 Low-energy collisions in two dimensions 9.4 Zeeman eﬀect and magnetic trapping 9.5 Interaction with the radiation ﬁeld and optical traps

130 130 132 141 143 148

PART II 10 The 10.1 10.2 10.3 10.4 10.5 10.6 10.7

Ideal Bose Gas in the Harmonic Trap Condensate fraction and critical temperature Density of single-particle states and thermodynamics Density and momentum distribution Thermodynamic limit Release of the trap and expansion of the gas Bose–Einstein condensation in deformed traps Adiabatic formation of BEC with non-harmonic traps

153 153 156 158 161 161 163 164

11 Ground State of a Trapped Condensate 11.1 An instructive example: the box potential 11.2 Interacting condensates in harmonic traps: density and momentum distribution 11.3 Energy, chemical potential, and virial theorem 11.4 Finite-size corrections to the Thomas–Fermi limit 11.5 Beyond-mean-ﬁeld corrections 11.6 Attractive forces

168 168

12 Dynamics of a Trapped Condensate 12.1 Collective oscillations 12.2 Repulsive forces and the Thomas–Fermi limit 12.3 Sum rule approach: from repulsive to attractive forces 12.4 Finite-size corrections to the Thomas–Fermi limit 12.5 Beyond-mean-ﬁeld corrections 12.6 Large-amplitude oscillations 12.7 Expansion of the condensate 12.8 Dynamic structure factor 12.9 Collective versus single-particle excitations

184 184 187 193 196 196 198 200 202 213

170 173 175 180 182

Contents

ix

13 Thermodynamics of a Trapped Bose Gas 13.1 Role of interactions, scaling, and thermodynamic limit 13.2 The Hartree–Fock approximation 13.3 Shift of the critical temperature 13.4 Critical region near Tc 13.5 Below Tc 13.6 Equation of state and density proﬁles 13.7 Collective oscillations at a ﬁnite temperature

217 217 220 223 226 228 233 236

14 Superﬂuidity and Rotation of a Trapped Bose Gas 14.1 Critical velocity of a superﬂuid 14.2 Moment of inertia 14.3 Scissors mode 14.4 Expanding a rotating condensate 14.5 Rotation at higher angular velocities 14.6 Quantized vortices 14.7 Vortices, angular momentum, and collective oscillations 14.8 Stability and precession of the vortex line 14.9 Quantized vortices and critical velocity in a toroidal trap

238 238 241 245 247 248 252 259 266 269

15 Coherence, Interference, and the Josephson Eﬀect 15.1 Coherence and the one-body density matrix 15.2 Interference between two condensates 15.3 Double-well potential and the Josephson eﬀect 15.4 Quantization of the Josephson equations 15.5 Decoherence and phase spreading 15.6 Boson Hubbard Hamiltonian

272 273 276 284 290 296 297

PART III 16 Interacting Fermi Gases and the BCS–BEC Crossover 16.1 The ideal Fermi gas 16.2 Dilute interacting Fermi gases 16.3 The weakly repulsive Fermi gas 16.4 Gas of composite bosons 16.5 The BCS limit of a weakly attractive gas 16.6 Gas at unitarity 16.7 The BCS–BEC crossover 16.8 The Bogoliubov–de Gennes approach to the BCS–BEC crossover 16.9 Equation of state, momentum distribution, and condensate fraction of pairs

305 305 307 307 309 311 313 319 323

17 Fermi Gas in the Harmonic Trap 17.1 The harmonically trapped ideal Fermi gas 17.2 Equation of state and density proﬁles 17.3 Momentum distribution

333 333 336 339

328

x

Contents

18 Tan 18.1 18.2 18.3 18.4 18.5 18.6

Relations and the Contact Parameter Wave function of a dilute Fermi gas near a Feshbach resonance Tails of the momentum distribution Dependence of energy on scattering length Relation between the energy and the momentum distribution Static structure factor The contact of a harmonically trapped gas

341 341 342 344 347 348 350

19 Dynamics and Superﬂuidity of Fermi Gases 354 19.1 Hydrodynamics at zero temperature: sound and collective oscillations 354 19.2 Expansion of a superﬂuid Fermi gas 360 19.3 Phonon versus pair-breaking excitations and Landau’s critical velocity 362 19.4 Dynamic structure factor 365 19.5 Radiofrequency transitions 366 19.6 Two-ﬂuid hydrodynamics: ﬁrst and second sound 370 19.7 Rotations and vortices 376 20 Spin-polarized Fermi Gases 20.1 Magnetic properties of the weakly repulsive Fermi gas 20.2 Superﬂuidity and magnetization 20.3 Phase separation at unitarity 20.4 Phase separation in harmonic traps at unitarity 20.5 The Fermi polaron

383 383 385 387 390 394

PART IV 21 Quantum Mixtures and Spinor Gases 21.1 Mixtures of Bose–Einstein condensates 21.2 Spinor Bose–Einstein condensates 21.3 Coherently coupled Bose–Einstein condensates 21.4 Synthetic gauge ﬁelds and spin-orbit coupling 21.5 Fermi–Bose mixtures

401 401 407 409 414 424

22 Quantum Gases in Optical Lattices 22.1 Single-particle properties in an optical lattice 22.2 Equilibrium properties of a Bose–Einstein condensate 22.3 Localization in one-dimensional quasiperiodic potentials 22.4 Equilibrium properties of a Fermi gas in a lattice 22.5 Bloch oscillations 22.6 Elementary excitations of BEC gases in an optical lattice 22.7 Centre-of-mass oscillation of a Fermi gas in an optical lattice 22.8 Dimer formation in periodic potentials 22.9 Quantum ﬂuctuations in optical lattices and the Bose– Hubbard model

428 428 432 437 440 442 445 451 452

23 Quantum Gases in Pancake and Two-dimensional Regimes 23.1 From three-dimensional pancakes to the two-dimensional regime 23.2 Two-dimensional Bose gas at ﬁnite temperatures

459 460 465

454

Contents

23.3 23.4

Fast-rotating Bose gases and the lowest Landau level regime Two-dimensional Fermi gas: the BEC–BCS crossover

xi

471 475

24 Quantum Gases in Cigar and One-dimensional Regimes 24.1 Bose gas: from three-dimensional radial cigars to the one-dimensional mean-ﬁeld regime 24.2 Solitons and vortical conﬁgurations in cigar traps 24.3 Phase ﬂuctuations and long-range behaviour of the oﬀ-diagonal one-body density 24.4 Lieb–Liniger theory: from the one-dimensional mean ﬁeld to the Tonks–Girardeau limit 24.5 Dynamic structure factor and superﬂuidity 24.6 One-dimensional Fermi gas

482

25 Dipolar Gases 25.1 The dipole–dipole force 25.2 Harmonic trapping and stability of dipolar BEC gases 25.3 Dynamic behaviour of dipolar gases 25.4 Dipolar Fermi gases

512 512 516 521 525

References

527

Index

551

482 487 492 495 503 506

1 Introduction After the experimental realization of Bose–Einstein condensation in dilute atomic gases achieved in 1995, the study of quantum gases in conditions of high degeneracy has become an emerging ﬁeld of physics, attracting the interest of scientists from diﬀerent areas. The basic idea of Bose–Einstein condensation (BEC) dates back to 1925 when A. Einstein, on the basis of a paper of the Indian physicist S. N. Bose (1924) devoted to the statistical description of the quanta of light, predicted the occurrence of a phase transition in a gas of noninteracting atoms. This phase transition is associated with the condensation of atoms in the state of lowest energy and is the consequence of quantum statistical eﬀects. For a long time these predictions had no practical impact. In 1938 F. London, immediately after the discovery of superﬂuidity in liquid helium (Kapitza, 1938; Allen and Misener, 1938), had the intuition that superﬂuidity could be a manifestation of Bose–Einstein condensation. The ﬁrst self-consistent theory of superﬂuids was developed by Landau in 1941 in terms of the spectrum of elementary excitations of the ﬂuid. This yielded the formulation of two ﬂuid hydrodynamics, an idea ﬁrst suggested by Tisza in 1940. In 1947 Bogoliubov developed the ﬁrst microscopic theory of interacting Bose gases, based on the concept of Bose– Einstein condensation. After Landau and Lifshitz (1951), Penrose (1951), and Penrose and Onsager (1956) introduced the concept of the nondiagonal long-range order and discussed its relationship with BEC, intense theoretical work was developed, aimed to better understand the relationship between BEC and superﬂuidity. Over the same period, the experimental studies on superﬂuid helium became more and more reﬁned, conﬁrming Landau’s predictions for the excitation spectrum and providing the ﬁrst measurements of the condensate fraction through the determination of the momentum distribution. An important development in the ﬁeld took place with the prediction of quantized vortices by Onsager (1949) and Feynman (1955), and with their discovery in experiments by Hall and Vinen (1956). The experimental studies on dilute atomic gases were developed much later, from the 1970s, proﬁting from new techniques developed in atomic physics based on magnetic and optical trapping and advanced cooling mechanisms. The ﬁrst studies were focused on spin-polarized hydrogen that was considered, because of its light mass and stability in gas phase down to zero temperature, the most natural candidate for realizing Bose–Einstein condensation. In a series of experiments hydrogen atoms were ﬁrst cooled in a dilution refrigerator, then trapped by a magnetic ﬁeld, and then further cooled by evaporation, coming very close to BEC. In the 1980s laser based techniques

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

2

Introduction

such as laser cooling and magneto-optical trapping, were developed to cool and trap neutral atoms. Alkali atoms are well suited to laser-based methods because their optical transition can be excited by available lasers and because they have a favourable internal energy-level structure for cooling to very low temperatures. Once they are trapped, their temperature can be lowered further by evaporative cooling. By combining the diﬀerent cooling techniques, the experimental teams of Cornell and Wieman at Boulder and of Ketterle at MIT eventually succeeded in 1995 in reaching the temperatures and the densities required to observe BEC in vapours of 87 Rb (Anderson et al., 1995) and 23 Na (Davis et al., 1995) (see Figure 1.1). In the same year, the ﬁrst signatures of the occurrence of Bose–Einstein condensation in vapours of 7 Li were also reported (Bradley et al., 1995). Bose–Einstein condensation was later achieved in spin-polarized hydrogen (Fried et al., 1998), in metastable 4 He (Robert et al., 2001 and Periera Dos Santos et al., 2001), and in 41 K (Modugno et al., 2001), as well as in a multitude of other atoms. At the same time, the study of interacting Fermi gases has also become a very popular research subject and has attracted increasing interest from both the experimental and theoretical communities, especially after the ﬁrst experimental achievement of Bose–Einstein condensation in a molecular gas of interacting fermions, realized by Greiner et al. (2003) with 40 K and by Zwierlein et al. (2003), Bourdel et al. (2003), Bartenstein et al. (2004a), and Partridge et al. (2005) with 6 Li (see Figure 1.2).

Figure 1.1 Images of the velocity distribution of rubidium atoms in the experiment by Anderson et al. (1995), taken by means of the expansion method. The left frame corresponds to a gas at a temperature just above condensation; the centre frame, just after the appearance of the condensate; and the right frame, after further evaporation leaves a sample of almost pure condensate. From Cornell (1996). Reprinted courtesy of the National Institute of Standards and Technology, US Department of Commerce.

Introduction

3

Using tunable Feshbach resonances, continuous crossover between the BardeenCooper-Schriﬀer superﬂuid state of weakly interacting fermions and BEC of fermionic molecules (BCS–BEC crossover) was investigated. Important experimental results have later conﬁrmed the superﬂuid behaviour of these ultracold interacting Fermi gases as the occurrence of quantized vortices (Zwierlein et al., 2005b), the anomalous behaviour of speciﬁc heat near the superﬂuid transition (Ku et al., 2012), and the propagation of second sound (Sidorenkov et al., 2013). From the theoretical side, the study of the superﬂuid phase in interacting Fermi gases and of the BCS–BEC crossover is deeply connected with the phenomenon of superconductivity. First eﬀorts started with the work by Eagles (1969), where it was pointed out that for large attraction between electrons the equations of BCS theory describe pairs of small size with a binding energy independent of density. A thorough discussion of the generalization of the BCS approach to describe the crossover in terms of the scattering length was presented in the seminal paper by Leggett (1980). This work concerned ground-state properties and

(a)

(b) 2.0

2.0

1.5

1.5

1.0

1.0

0.5

0.5

0.0

0.0 –200 –100 0 100 200 position (μm)

–200 –100 0 100 200 position (μm)

Figure 1.2 Emergence of a molecular BEC in an ultracold Fermi gas of 40K atoms, observed in time-of-ﬂight absorption images. The density distribution on the left-hand side was taken for a weakly interacting Fermi gas which was cooled down to 19% of the Fermi temperature. After ramping across the Feshbach resonance no BEC was observed as the sample was too hot. The density distribution on the right-hand side was observed for a colder sample. Here the ramp across the Feshbach resonance resulted in a bimodal distribution, revealing the presence of a molecular BEC. From Greiner et al. (2003). Reprinted by permission from Nature, 426, c 2003, Macmillan Publishers Ltd. 537;

4

Introduction

was later extended to ﬁnite temperatures by Nozi`eres and Schmitt-Rink (1985) and by S´ a de Melo, Randeria, and Engelbrecht (1993) to calculate the critical temperature for the onset of superﬂuidity. These theories describe the properties of the many-body conﬁgurations along the BCS–BEC crossover in terms of a single parameter related to interactions, and the dimensionless combination kF a where a is the s-wave scattering length and kF is the Fermi wavevector. The predicted values for the critical temperature show that Tc can easily reach values of the order of the Fermi temperature in a wide interval of values of kF |a|. For this reason one often speaks of high-Tc Fermi superﬂuidity. The study of fermionic systems is in many respects complementary to that of bosons. Quantum statistics plays a major role at low temperature, according to the pioneering works by Fermi (1926) and Dirac (1926). Although the relevant temperature scale providing the onset of quantum degeneracy is the same in both cases, being of the order of kB Tdeg ∼ 2 n2/3 /m where n is the gas density and m is the mass of the atoms, the physical consequences of quantum degeneracy are diﬀerent. In the Bose case quantum statistical eﬀects are associated with the occurrence of a phase transition to the Bose–Einstein condensed phase. Conversely, in a non-interacting Fermi gas the quantum degeneracy temperature only corresponds to a smooth crossover between a classical and a quantum behaviour. In contrast to the Bose case, the occurrence of a superﬂuid phase in a Fermi gas can only be due to the presence of interactions. From the many-body point of view, the study of Fermi superﬂuidity opens a diﬀerent and richer class of questions which will be discussed in Part III of this volume. A further important diﬀerence between Bose and Fermi gases concerns the collisional processes; in particular, in a single-component Fermi gas s-wave scattering is inhibited due to the Pauli exclusion principle. This eﬀect has important consequences on the cooling mechanisms based on evaporation, where thermalization plays a crucial role. The availability of Feshbach resonances, with the possibility of changing the value and even the sign of the scattering length by simply tuning an external magnetic ﬁeld, has enabled the investigation of strongly interacting regimes of fermionic atoms working near the resonance where the scattering length can take very large values. In contrast to Bose gases in the case of fermions three-body losses are inhibited by the Pauli exclusion principle, leading to a greater stability of the gas and to the possibility of realizing the so-called unitary regime of inﬁnite scattering length where the system exhibits a universal behaviour, independent of the details of the interatomic potential (Bertsch, 1999), and where the gas is at the same time dilute and strongly interacting, the interparticle distance being larger than the range of the force but smaller than the scattering length. At low temperature Bose–Einstein condensates and interacting Fermi gases share important analogies due to their superﬂuid nature; these notable phenomena will be discussed in detail in this volume. From a many-body point of view, superﬂuidity is an important consequence of the existence of long-range order in the nondiagonal one-body (for bosons) and two-body (for fermions) densities. The aim of the present volume is to present an introduction to the most relevant concepts related to Bose–Einstein condensed and interacting Fermi gases, with special emphasis on their superﬂuid behaviour.

Introduction

5

Part I starts with chapter 2, where we introduce the concept of nondiagonal longrange order, which is a basic ingredient of BEC. In Chapter 3 we summarize the main features of the ideal Bose gas, one of the few soluble models of quantum statistical mechanics exhibiting phase transition. Chapter 4 is devoted to describing the Bogoliubov theory of interacting gases, where the combined eﬀect of BEC and two-body interactions results in the propagation of sound waves. In chapter 5 we develop the theory of inhomogeneous interacting Bose gases on the basis of a classical description of the order parameter (Gross-Pitaevskii theory). In Chapter 6 we discuss the general properties of superﬂuids; the main equations governing superﬂuids can be obtained microscopically starting from the theory of dilute gases, but they have a much wider range of applicability, including the physics of dense superﬂuids. Chapter 7 presents an overview of the important formalism of linear response theory, while Chapter 8 summarizes some key features of superﬂuid helium, with special emphasis on those quantities (excitation spectrum, quantized vortices) where a useful comparison can be made with the physics of dilute Bose gases. In Chapter 9 we provide a brief summary of the atomic properties allowing for the magnetic and optical trapping of dilute gases. Part II is devoted to the physics of trapped Bose–Einstein condensed gases. Chapter 10 is devoted to the study of the ideal Bose gas conﬁned in a harmonic trap, where important predictions can be made, especially concerning the critical temperature for Bose–Einstein condensation. In the following chapters we apply the general theory of inhomogeneous interacting gases to the case of harmonic traps, deriving results for the equilibrium (Chapter 11) and dynamic (Chapter 12) properties at zero temperature. Chapter 13 is instead devoted to discussing the eﬀects of the interactions on the thermodynamic behaviour of these systems. The rotational properties of trapped gases are discussed in Chapter 14, with special emphasis to the behaviour of quantized vortices. In Chapter 15 we discuss some coherence properties exhibited by Bose–Einstein condensed gases, including interference phenomena and Josephson-like eﬀects. Part III of this volume is devoted to the study of interacting Fermi gases at low temperatures and in particular of their superﬂuid properties. In Chapter 16 we provide a general discussion of the BCS–BEC crossover. In Chapter 17 we discuss some properties of harmonically trapped Fermi gases, while in Chapter 18 we focus on some important thermodynamic relations and on the role of the so called contact parameter. In Chapter 19 we present some dynamic and superﬂuid features of fermionic gases, while Chapter 20 is devoted to spin-polarized Fermi gases. Part IV treats topics of joint interest for both Bose and Fermi gases: quantum mixtures (Chapter 21); the physics in the presence of optical lattices (Chapter 22); low dimensional conﬁgurations (Chapters 23 and 24); and dipolar gases (Chapter 25). This volume covers only part of the important subjects related to the physics of Bose–Einstein condensation and Fermi gases. It develops and extends the theoretical investigation presented in the review papers by Dalfovo et al. (1999) and Giorgini et al. (2008), and we consequently refer to other text books or review papers for the subjects which are not discussed, or are only marginally mentioned here. An interdisciplinary discussion on BEC, covering diﬀerent disciplines of physics, can be found

6

Introduction

in the proceedings of the Levico conference of 1993 (Griﬃn et al., 1995). A theoretical presentation of the physics of Bose–Einstein condensation in atomic gases can be found in Pethick and Smith (2008), while a comprehensive discussion of ultracold atoms in optical lattices can be found in Lewenstein et al. (2012). For other reviews we refer to the paper by Leggett (2001) and to the more recent review article by Bloch et al. (2008). A collection of experimental and theoretical papers on Bose and Fermi gases is provided by the lecture notes of three Varenna Schools (Inguscio et al., 1999, 2008, and 2014), the 2010 Les Houches School (Salomon et al., 2013), and Zwerger (ed.) (2012) devoted to interacting Fermi gases. For a comprehensive discussion on polaritons and interacting photons in nonlinear optical systems—systems which share important analogies with atomic Bose gases and exhibit characteristic superﬂuid phenomena—we address the reader to the recent review paper by Carusotto and Ciuti (2013). Bose–Einstein condensation in quantum magnets has also been the object of systematic experimental and theoretical research (for a recent review see, for example, Zapf et al., 2014). Other reviews and books focused on more speciﬁc subjects will be mentioned in the various chapters of this volume.

Part I

2 Long-range Order, Symmetry Breaking, and Order Parameter Long-range order, symmetry breaking, and order parameter are key concepts underlying the phenomenon of Bose–Einstein condensation (BEC). These concepts are usually discussed in the context of uniform macroscopic systems. Since an important part of this book is devoted to discussing BEC in atomic gases conﬁned in traps, it is useful to develop from the very beginning a formalism accounting for the new features exhibited by nonuniform systems and to discuss to what extent these fundamental concepts of statistical mechanics can be extended to ﬁnite samples. The concept of long-range order and Bose–Einstein condensation also plays a crucial role in Fermi gases. Noninteracting fermions do not exhibit the phenomenon of Bose–Einstein condensation, but interactions can give rise to pairing eﬀects which appear, in the superﬂuid phase, in a characteristic long range order exhibited by the two-body density matrix. This behaviour will be discussed in Section 16.7.

2.1

One-body density matrix and long-range order

Let us start our discussion by introducing the one-body density matrix ˆ † (r)Ψ(r ˆ ), n(1) (r, r ) = Ψ

(2.1)

ˆ ˆ † (r) (Ψ(r)) is the ﬁeld operator creating (annihilating) a particle at point r. where Ψ The meaning of the average · · · will be discussed later. Since n(1) (r, r ) = (n(1) (r , r))∗ the matrix n(1) is hermitian. Equation (2.1) provides a very general deﬁnition which applies to any system, independently of statistics, in as well as out of equilibrium. In the latter case the density matrix will of course depend on time. For a system of bosons the ﬁeld operators of eqn (2.1) satisfy the well-known commutation relations ˆ ˆ † (r )] = δ(r − r ), [Ψ(r), ˆ ˆ )] = [Ψ ˆ † (r), Ψ ˆ † (r )] = 0 . [Ψ(r), Ψ Ψ(r

(2.2)

The one-body density matrix (2.1) contains information on important physical observables. By setting r = r one ﬁnds the diagonal density of the system: ˆ ˆ † (r)Ψ(r) = n(1) (r, r). n(r) = Ψ

(2.3)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

10

Long-range Order, Symmetry Breaking, and Order Parameter

The total number of particles is then N = drn(r) = drn(1) (r, r). This equation deﬁnes the normalization of the one-body density matrix. The density matrix (2.1) also determines the momentum distribution ˆ † (p)Ψ(p), ˆ n(p) = Ψ

(2.4)

−3/2

ˆ ˆ where Ψ(p) = (2π) dr exp[−ip · r/¯ h]Ψ(r) is the ﬁeld operator in momenˆ tum representation. By inserting the above expression for Ψ(p) into eqn (2.4) one immediately ﬁnds the relation s −ip·s/ 1 s (1) , R − e n(p) = R + dRdsn (2.5) (2π)3 2 2 between the one-body density matrix and the momentum distribution, where s = r − r and R = (r + r )/2. The momentum distribution has the same normalization dpn(p) = N as the diagonal density, ﬁxed by the total number of particles. If the system occupies a pure state, described by the N -body wave function Ψn (r1 , . ., rN ), then the average (2.1) is taken following the standard rules of quantum mechanics and the one-body density matrix can be written as n(1) (r, r ) = N dr2 . . . .drN Ψ∗n (r, r2 , . ., rN )Ψn (r , r2 , . ., rN ), (2.6) n involving the integration over the N − 1 variables r2 , . . . rN . The many-body wave function Ψn (r1 , . . . , rN ) is here normalized to 1. The above formalism is easily extended to include additional degrees of freedom, like spin. For the more general case of a statistical mixture, expression (2.6) should be averaged according to the probability of a system occupying the diﬀerent states n. The most important example is a system in thermodynamic equilibrium. In this case the states Ψn are eigenstates of the Hamiltonian with energy En and the weight of each state is ﬁxed by the factor exp(−En /kB T ), so that the density matrix becomes n(1) (r, r ) =

1 −En /kB T (1) e nn (r, r ), n Q

(2.7)

where Q = Σn exp(−En /kB T ) is the partition function. Let us ﬁrst consider the case of a uniform and isotropic system of N particles occupying a volume V in the absence of external potentials. In the thermodynamic limit, where N, V → ∞ with the density n = N/V kept ﬁxed, the one-body density depends only on the modulus of the relative variable s = r − r : n(1) (r, r ) = n(1) (s) and one can write 1 n(1) (s) = dpn(p)eip·s/ . (2.8) V For a normal system the momentum distribution has a smooth behaviour at small momenta and consequently the one-body density vanishes when s → ∞. The situation is diﬀerent in the presence of Bose–Einstein condensation where, due to

One-body density matrix and long-range order

11

the macroscopic occupation of the single particle state with momentum p = 0, the momentum distribution contains a delta-function term n(p) = N0 δ(p) + n ˜ (p)

(2.9)

whose weight N0 is proportional to the total number of particles. The quantity N0 /N ≤ 1 is called the condensate fraction. By taking the Fourier transform (2.8) one ﬁnds that, in the presence of BEC, the one-body density matrix does not vanish at large distances but approaches a ﬁnite value: n(1) (s)s→∞ → n0 ,

(2.10)

ﬁxed by the parameter n0 = N0 /V . This behaviour was pointed out by Landau and Lifshitz (1951), Penrose (1951), and Penrose and Onsager (1956), and is often referred to as oﬀ-diagonal long-range order, since it involves the nondiagonal components (r = r ) of the one-body density (2.1). The above considerations also hold in the presence of interactions which of course aﬀect the value of the parameter n0 . For example, while in the ideal gas all the particles are in the condensate at T = 0 and N0 = N, in the presence of interactions one has N0 < N even at T = 0. The condensate fraction N0 /N depends on the temperature of the sample and vanishes above the critical temperature Tc for Bose–Einstein condensation where the system exhibits a normal behaviour. In Figure 2.1 we show the typical behaviour of n(1) (s) at diﬀerent temperatures. For completeness it is also useful to carry out the low-s expansion of the one-body density matrix. From eqn (2.8) one immediately ﬁnds the result 1 2 s2 (1) n (s)s→0 = n 1 − pz 2 + . . . , (2.11) 2 where we have chosen s oriented along z and we have deﬁned p2z = N −1 dpn(p)p2z .

n

n(1)(s)

T < Tc n0 T > Tc

s

Figure 2.1 Oﬀ-diagonal one-body density as a function of the relative distance s. For temperatures below the critical temperature, n(1) (s) approaches, for large s, the value n0 = N0 /V , where N0 is the number of particles in the condensate. At s = 0, n(1) (s) coincides with the diagonal density n = N/V .

12

Long-range Order, Symmetry Breaking, and Order Parameter

The long-range order exhibited by the one-body density matrix is strongly connected with the behaviour of its eigenvalues ni deﬁned by the solution of the eigen equation dr n(1) (r, r )ϕi (r ) = ni ϕi (r). (2.12) The solutions of (2.12) provide a natural basis of ortho-normalized single-particle wave functions: ϕ∗i ϕj dr = δij . By multiplying (2.12) by ϕ∗i (r) and integrating over r, one ﬁnds the normalization condition Σi ni = N which follows from the completeness relation Σi ϕ∗i (r)ϕ∗i (r ) = δ(r − r ) and from the normalization of the diagonal density. Notice that the single-particle wave functions ϕi are well deﬁned not only for an ideal gas, but also for interacting and nonuniform systems. The knowledge of the functions ϕi and of the eigenvalues ni permits us to write the density matrix in the useful diagonalized form: n(1) (r, r ) = Σi ni ϕ∗i (r)ϕi (r ).

(2.13)

In the language of second quantization (see eqn (2.18)) the eigenvalues ni provide the single-particle occupation numbers relative to the single-particle states ϕi . Bose–Einstein condensation occurs when one of the single-particle states (hereafter called the condensate, i = 0) is occupied in a macroscopic way, i.e. when ni = 0 ≡ N0 is a number of order N , while the other single-particle states have a microscopic occupation of order 1. In this case eqn (2.13) can be conveniently rewritten in the separated form n(1) (r, r ) = N0 ϕ∗0 (r)ϕ0 (r ) + ni ϕ∗i (r)ϕi (r ). (2.14) i=0

In the thermodynamic limit (N → ∞) the sum with i = 0 can be replaced by a proper integration which consequently tends to zero at large distances s = |r − r |. Vice versa, the contribution of the condensate remains ﬁnite up to distances |r − r | ﬁxed by the extension of the function ϕ0 . For uniform systems the solutions of (2.12) are plane waves 1 ϕpi (r) = √ eipi ·r/ , V

(2.15)

with the value of pi determined by the boundary conditions. In this case one ﬁnds a direct relation between the occupation numbers npi and the momentum distribution n(p). In fact, inserting (2.14) into (2.5) one ﬁnds the result n(p) = N0 δ(p) + npi δ(p − pi ), (2.16) pi =0

from which, by replacing the sum over the states pi = 0 with the integral V /(2π)3 dp, one immediately obtains eqn (2.9) with the identiﬁcation n ˜ (p) =

V np . (2π)3

(2.17)

Order parameter

13

If the system is not uniform the solutions of (2.12) are no longer plane waves and must be in general determined numerically. Provided N is suﬃciently large, the concept of Bose–Einstein condensation is also well deﬁned in this case, being associated with the macroscopic occupation of a single-particle state.

2.2

Order parameter

A major consequence of the diagonalization (2.13) is given by the possibility of identifying in an unambiguous way the single-particle wave functions ϕi for both interacting ˆ and nonuniform systems. These functions can be used to write the ﬁeld operator Ψ(r) in the form ˆ Ψ(r) = ϕi a ˆi . (2.18) i

a†i ) are the annihilation (creation) operators of a particle in the state ϕi and where a ˆi (ˆ obey the commutation relations [ˆ ai , a ˆ†j ] = δij , [ˆ ai , a ˆ†j ] = [ˆ a†i , a ˆ†j ] = 0.

(2.19)

Inserting eqn (2.18) into (2.1) and comparing with eqn (2.14) one ﬁnds that the expectation value of the operators a ˆ†j a ˆi is given by ˆ a†j a ˆi = δij ni . The wave function relative to the macroscopic eigenvalue N0 plays a crucial role in the theory of BEC and characterizes the so-called wave function of the condensate. It is useful to separate in the ﬁeld operator (2.18) the ‘condensate’ term i = 0 from the other components: ˆ Ψ(r) = ϕ0 (r)ˆ a0 +

ϕi (r)ˆ ai .

(2.20)

i=0

This equation provides the natural starting point for introducing the Bogoliubov approximation, which consists of replacing the operators a ˆ0 and a ˆ†0 with the c-number √ N0 . This is equivalent to ignoring the noncommutativity of the operators a ˆ0 and a ˆ†0 and is a good approximation for describing the macroscopic phenomena associated with BEC, where N0 = a†0 a0 1. In fact, the commutator between the operators a0 √ and a†0 is equal to 1, while the operators themselves are of order N0 . The Bogoliubov approximation is equivalent to treating the macroscopic component ϕ0 a ˆ0 of the ﬁeld operator (2.20) as a classical ﬁeld so that eqn (2.20) can be rewritten as ˆ ˆ Ψ(r) = Ψ0 (r) + δ Ψ(r), (2.21) √ ˆ = where we have deﬁned Ψ0 = N0 ϕ0 and δ Ψ i=0 ϕi ai . If one can neglect the nonˆ condensed component δ Ψ, as happens, for example, in dilute Bose gases at very low temperatures, then the ﬁeld operator coincides exactly with the classical ﬁeld Ψ0 and the system behaves like a classical object. This is the analogue of the classical limit of quantum electrodynamics where the classical electromagnetic ﬁeld entirely replaces the microscopic description of photons. Though the separation (2.21) is particularly

14

Long-range Order, Symmetry Breaking, and Order Parameter

useful in the case of dilute gases, where it is possible to obtain closed equations for the ﬁeld Ψ0 (see Chapter 5), it can also be employed in the case of strongly interacting systems like superﬂuid helium, its validity being guaranteed by the occurrence of a macroscopic occupation of a single-particle state (N0 1). The function Ψ0 (r) is called the wave function of the condensate and plays the role of an order parameter. It is a complex quantity, characterized by a modulus and a phase: Ψ0 (r) = |Ψ0 (r)|eiS(r) .

(2.22)

The modulus determines the contribution of the condensate to the diagonal density (2.3). The phase S(r) plays, as we will see, a major role in characterizing the coherence and superﬂuid phenomena. The order parameter (2.22) characterizes the Bose–Einstein condensed phase and vanishes above the critical temperature. As √ one can see from its deﬁnition (2.14), the order parameter Ψ0 = N0 ϕ0 is deﬁned only up to a constant phase factor. One can always multiply this function by the numerical factor eiα without changing any physical property. This reﬂects the gauge symmetry exhibited by all the physical equations of the problem. Making an explicit choice for the value of the order parameter (and hence for the phase) corresponds to a formal breaking of gauge symmetry. The Bogoliubov ansatz (2.21) for the ﬁeld operator can be interpreted by saying ˆ of the ﬁeld operator is diﬀerent from zero. This would that the expectation value Ψ not be possible if the states on the left and on the right had exactly the same number of particles. From a physical point of view, this symmetry breaking means that the condensate plays the role of a reservoir. Since N0 1 adding a particle in the condensate does not change the physical properties of the system. In other words the state |N containing N particles and the states |N + 1 ∝ a†0 |N and |N − 1 ∝ a0 |N are physically equivalent, apart from corrections of order 1/N0 . In conclusion, one can ˆ having in mind that the states on the left have one less particle in write Ψ0 = Ψ, ˆ † . If we take this the condensate than those on the right. Similarly, one has Ψ∗0 = Ψ average over stationary states, whose time dependence is governed by the law e−iEt/ , it is easy to see that the time dependence of the order parameter is given by the law Ψ0 (r, t) = Ψ0 (r)e−iμt/ ,

(2.23)

where μ = E(N ) − E(N − 1) ≈ ∂E/∂N is the chemical potential. It is interesting to remark that the time evolution of the order parameter is not governed by the energy, as happens with usual wave functions, but by the chemical potential which emerges as a key parameter in the physics of Bose–Einstein condensates.

3 The Ideal Bose Gas The quantum statistical description of the noninteracting Bose gas is a popular subject described in many text books of statistical mechanics. The ideal Bose gas provides the simplest example of realization of Bose–Einstein condensation and some of its predictions correctly describe important properties of actual systems. London (1938) ﬁrst had the intuition that important features of superﬂuid helium could be interpreted using the basic concepts of the ideal Bose gas. More recently the value of the critical temperature predicted by the ideal Bose gas has provided experimentalists with valuable guidance for reaching the BEC regime in the investigation of dilute atomic gases conﬁned in harmonic traps.

3.1

The ideal Bose gas in the grand canonical ensemble

In the following we will provide the quantum statistical description of the ideal Bose gas in the context of the grand canonical ensemble where the formalism becomes particularly simple. Let us recall that, in the grand canonical ensemble the probability to realize a conﬁguration with N particles in a state k with energy Ek is calculated as PN (Ek ) = eβ(μN

−Ek )

,

(3.1)

where β = 1/kB T and μ is the chemical potential of the reservoir with which the system is in thermal equilibrium. A major issue of statistical mechanics is the calculation of the grand canonical partition function

Z(β, μ) =

∞ N =0 k

PN (Ek ) =

∞

eβμN QN (β),

(3.2)

N =0

where QN = k e−βEk is the canonical partition function calculated for a system of N particles and the sum k includes a complete set of eigenstates of the Hamiltonian with energy Ek . The natural variables in the grand canonical ensemble are the temperature and the chemical potential, as well as the parameters needed to characterize the external constraints of mechanical nature. These latter parameters, which can be the volume of the sample or the oscillator frequency in the case of harmonic trapping, enter the grand partition function only through the eigenvalues Ek of the Hamiltonian and have not been explicitly indicated in eqn (3.2). From the knowledge of the grand

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

16

The Ideal Bose Gas

canonical partition function one can straightforwardly evaluate the thermodynamic behaviour of the system through the identiﬁcation Ω = −kB T ln Z

(3.3)

for the grand canonical potential Ω = E − T S − μN , where S=−

∂Ω ∂T

(3.4)

is the entropy of the system. The total number of particles N =−

∂Ω ∂μ

(3.5)

and the energy E =Ω−T

∂Ω ∂Ω −μ ∂T ∂μ

(3.6)

∞ coincide, ∞ respectively, with the grand canonical averages N =0 k N PN (Ek ) and E P (E ), calculated starting from (3.1). k N =0 k k N If the system is uniform and occupies a volume V , then the grand potential function Ω reduces to Ω = −P V,

(3.7)

where P is the pressure acting on the system, and hence directly provides the equation of state. Let us now consider a system described by the independent particle Hamiltonian (1) ˆ = ˆ H . (3.8) H i i

In this case the eigenstates k are deﬁned by specifying the set {ni } of the microscopic occupation numbers ni of the single-particle states, obtained by solving the Schr¨ odinger equation ˆ (1) ϕi (r) = i ϕi (r). H

(3.9)

In fact, using the formalism of second quantization, the state |k ∝ (a†0 )n0 (a†1 )n1 . . . |vac

(3.10)

speciﬁes in a complete way the many-body eigenstate of the Hamiltonian (3.8). Here a†i (ai ) are the particle creation (annihilation) operators relative to the i-th singleparticle state. They obey the commutation rule [ai , a†j ] = δij for bosons and the anticommutation rule {ai , a†j } = δij for fermions, while the state |vac is the vacuum of particles (ai |vac = 0).

The ideal Bose gas in the grand canonical ensemble

17

For the independent particle Hamiltonian (3.8) the grand canonical function (3.2) can be worked out exactly. In fact, in this case N = i ni and Ek = i i ni , where i are the single-particle eigenenergies determined by the solution of (3.9), and the grand partition function (3.2) can be written as Z=

(eβ(μ−0 ) )n0

n0

(eβ(μ−1 ) )n1 . . . ,

(3.11)

n1

where, in Bose statistics, the sum n extends over the values n = 0, 1, 2, . . . , while in the Fermi case it is limited to the values n = 0, 1. Notice that the sums in (3.11) have no restriction imposed by the total number of particles because the grand canonical sum (3.2) includes all the possible values of N . In the ideal Bose gas the sum (3.11) yields the following result for the grand canonical potential (3.3): Ω = kB T

ln(1 − eβ(μ−i ) ).

(3.12)

i

Using (3.5) one can easily evaluate the total number of particles N=

i

1 = n ¯i, exp[β(i − μ)] − 1 i

(3.13)

which can be written as the sum of the average occupation numbers n ¯i = −

∂ 1 ln Z = ∂βi exp[β(i − μ)] − 1

(3.14)

of each single-particle state. One can now easily evaluate all the other thermodynamic functions. For example, the energy and the entropy are given by E=

i

i exp[β(i − μ)] − 1

(3.15)

and S = [(1 + ni ) ln(1 + ni ) − ni ln ni ] kB i

=

i

β(i − μ) β(μ−i ) − ln(1 − e ) , exp[β(i − μ)] − 1

(3.16)

respectively. Result (3.14) provides the important physical constraint μ < 0 for the chemical potential of the ideal Bose gas where 0 is the lowest eigenvalue of the single-particle Hamiltonian H (1) . The violation of this inequality would result in a negative value for

18

The Ideal Bose Gas

the occupation number of the states with energy smaller than μ. When μ → 0 the occupation number N0 ≡ n ¯0 =

1 exp[β(0 − μ)] − 1

(3.17)

of the lowest energy state becomes larger and larger. This is actually the mechanism at the origin of Bose–Einstein condensation. Let us write the total number of particles as N = N0 + NT ,

(3.18)

where NT (T, μ) =

n ¯ i (T, μ)

(3.19)

i=0

is the number of particles out of the condensate, also called the thermal component of the gas. The value of NT , being proportional to the density of states, increases with the size of the system (see eqn (3.23) below). For a ﬁxed value of T , the function NT has a smooth behaviour as a function of μ and reaches its maximum Nc at μ = 0 (see Figure 3.1). The behaviour of N0 is very diﬀerent. In fact N0 is always of order 1, except when μ is close to 0 where N0 diverges. If the value of Nc = NT (T, μ = 0 ) is larger than N , then eqn (3.18) is satisﬁed for values of μ smaller than 0 and N0 is negligible with respect to N . Since the function Nc (T ) is an increasing function

N0(μ)

•

Nc

NT(μ)

μ

ε0

Figure 3.1 Ideal gas model. The number of particles out of the condensate (NT , solid line) and in the condensate (N0 , dashed line) as a function of the chemical potential, for a ﬁxed value of T . The actual value of μ is ﬁxed by the normalization condition N = N0 + NT . If N > Nc the solution is given by μ ∼ 0 and the system exhibits Bose–Einstein condensation (N0 /N = 0) in the thermodynamic limit.

The ideal Bose gas in the box

19

of T , this scenario takes place for temperatures higher than the critical temperature Tc deﬁned by the relation NT (Tc , μ = 0 ) = N.

(3.20)

If instead Nc (T ) is smaller than N (or, equivalently, T < Tc ), then the contribution of the condensate is crucial in order to satisfy the normalization condition (3.18) and the value of μ will approach 0 in the thermodynamic (large N ) limit. The temperature Tc then deﬁnes the critical temperature below which the phenomenon of Bose–Einstein condensation, i.e. the macroscopic occupation of a single-particle state, takes place.

3.2

The ideal Bose gas in the box

Let us apply the formalism described above to the problem of an ideal Bose gas conﬁned in a box of volume V . In this case the single-particle Hamiltonian has the simple form H (1) =

p2 , 2m

(3.21)

whose solutions, using cyclic boundary conditions ϕ(x, y, z) = ϕ(x + L, y, z) etc., with L = V 1/3 , are plane waves 1 ϕp = √ eip·r/ V

(3.22)

with energy = p2 /2m and momentum p = 2πn/L where n is a vector whose components nx , ny , nz are 0 or ± integers. The lowest eigenvalue has zero energy (0 = 0) so potential must be always negative. By making the replacement that the chemical 3 → V /(2πh ) dp to evaluate the sum over the states with p = 0 and using the p transformation p2 = 2mkB T x, the number of atoms out of the condensate (thermal depletion of the condensate) can be written in the form NT =

p=0

1 V = 3 g3/2 (eβμ ), exp[β(p2 /2m − μ)] − 1 λT

(3.23)

where 2π2 mkB T

λT =

(3.24)

is the thermal wave length and 2 g3/2 (z) = √ π

0

∞

dxx1/2

1 z −1 ex − 1

(3.25)

20

The Ideal Bose Gas

is a special case of the more general class of Bose functions gp (z) =

1 Γ(p)

∞

∞

dxxp−1

0

z 1 = . −1 x z e −1 p

(3.26)

=1

Here z = exp(βμ) is the so-called fugacity and Γ(p) is the factorial function (p − 1)!. The functions gp (z) satisfy the recurrence relations gp (z) = z

dgp+1 (z) . dz

(3.27)

Notice that the replacement of the sum with an integral in the derivation of (3.23)–(3.25) is justiﬁed only if the thermal energy kB T is much larger than the energy spacing between single-particle levels, i.e. if kB T h2 /2mV 2/3 . Notice also that the above results have been derived in three dimensions and that the behaviour of the corresponding functions is very diﬀerent in lower dimensions. The criterion for BEC discussed in the previous section yields the following result for the critical temperature (3.20) for Bose–Einstein condensation: kB Tc =

2π2 m

n g3/2 (1)

2/3 (3.28)

with g3/2 (1) = 2.612. Equation (3.28) shows that the critical temperature of an ideal gas conﬁned in a three-dimensional box is fully determined by the density n = N/V and by the mass of the constituents. For temperatures T > Tc the value of the chemical potential is obtained by setting NT = N in eqn (3.23), which becomes g3/2 (z) = λ3T n.

(3.29)

For temperatures below Tc eqn (3.18) is instead solved by setting μ = 0 in NT . In this case, using result (3.28), eqn (3.23) yields NT =

mkB T 2π2

3/2

g3/2 (1)V =

and the number of particles in the condensate

N0 (T ) = N 1 −

T Tc

T Tc

3/2 N

(3.30)

3/2 (3.31)

becomes macroscopic (Figure 3.2). Analogously, for a ﬁxed value of T one can deﬁne a critical volume vc =

λ3T . g3/2 (1)

(3.32)

The ideal Bose gas in the box

21

1.2 1

1−

T Tc

3/2

N0 /N

0.8 0.6 0.4 0.2 0

0

0.2

0.4

0.6 T /Tc

0.8

1

1.2

Figure 3.2 Condensate fraction N0 /N versus temperature for a uniform ideal Bose gas. The condensate fraction is diﬀerent from zero below Tc where the system exhibits Bose–Einstein condensation.

It is then immediate to see that Bose–Einstein condensation takes place if the speciﬁc volume v = 1/n is smaller than vc . Result (3.30) reﬂects the saturation property of the Bose–Einstein condensed gas. In fact, it shows that, for a given temperature, the number NT of thermal atoms does not depend on the total number N , but only on the volume of the box. Adding more atoms to the system will consequently result in an increase of N0 , but not of NT . The saturation property of a Bose–Einstein condensed gas conﬁned in a box has recently been conﬁrmed in experiments by Schmidutz et al. (2014). Equation (3.30) shows that at low temperatures the number of particles NT out of the condensate tends to zero. This result is consistent with the fact that in the ideal gas model (3.9) the ground state is obtained by putting all the particles in the lowest single-particle state (N0 = N ). However, one should not confuse the microscopic criterion kB T (1 − 0 ) =

h2 2mV 2/3

(3.33)

for the system being in the ground state with the condition NT N which requires the weaker condition T Tc . Here 1 is the energy of the ﬁrst single-particle excited state. For large samples the condition h2 /(2mV 2/3 ) kB T kB Tc can actually be well satisﬁed, so that in this case Bose–Einstein condensation (N0 of the order of N ) also takes place for these macroscopic values of T . The use of macroscopic values of T is actually crucial in order to treat the thermal component as a continuum of excitations and to replace the sum over the single-particle states with an integral in the evaluation of the thermodynamic functions. Another question concerns the exact value of μ which

22

The Ideal Bose Gas

was set equal to 0 in the derivation of result (3.23) for NT . The actual value of μ can be evaluated from the relation kB T 1 0 − μ = kB T ln 1 + (3.34) N0 N0 following from eqn (3.17) and showing that μ → 0 only in the thermodynamic limit where N0 → ∞. Replacing μ with 0 in the evaluation of NT is then justiﬁed only if (1 − 0 ) (0 − μ) ∼ kB T /N0 , i.e. if the condition N0 kB T V 2/3 2m/h2 is satisﬁed. All the thermodynamic functions can now be easily evaluated. The energy (3.15) takes the value E=

3 V kB T 3 g5/2 (1) 2 λT

(3.35)

E=

V 3 kB T 3 g5/2 (z) 2 λT

(3.36)

for T < Tc , and

for T > Tc , where the function g5/2 (z) is given by ∞ 1 4 √ g5/2 (z) = dxx3/2 −1 x 3 π 0 z e −1

(3.37)

and corresponds to the p = 5/2 Bose function (3.26). At z = 1 one has g5/2 (1) = 1.342. Simple results are also obtained for the speciﬁc heat CV = ∂E/∂T for which one ﬁnds the result 15 v CV = g5/2 (1) kB N 4 λ3T

(3.38)

15 v 9 g3/2 (z) CV = 3 g5/2 (z) − kB N 4 λT 4 g1/2 (z)

(3.39)

for T < Tc and

for T > Tc . The speciﬁc heat has a typical cusp at Tc but is a continuous function at the transition (see Figure 3.3). The Bose function g1/2 (z) in fact diverges as z → 1. The continuity of the speciﬁc heat is not, however, a general rule of the ideal Bose gas. For example, in the case of harmonic trapping the speciﬁc heat predicted by the ideal Bose gas model exhibits a discontinuity at T = Tc (see Chapter 10). Using the thermodynamic relation P =

2E , 3V

(3.40)

holding for ideal gases in three dimensions, and results (3.35) and (3.36) for the energy of the gas, one can also easily calculate the equation of state P (V ). It is worth noticing

The ideal Bose gas in the box

23

CV / N k

2

1

0

0

0.5

1

1.5 T /Tc

2

2.5

3

Figure 3.3 Speciﬁc heat of the uniform ideal Bose gas versus temperature. For large T the curve approaches the classical value 3/2. The curve exhibits a cusp at T = Tc .

that in the Bose–Einstein condensed phase (T < Tc ) the energy increases linearly with the volume (see eqn (3.35)) so that the pressure of the gas, which takes the form P =

kB T g5/2 (1), λ3T

(3.41)

does not depend on the volume. This implies that in the BEC phase the isothermal compressibility κT = (∂n/∂P )T /n, with n = N/V the density of the gas, is inﬁnite. This pathological feature is changed by the inclusion of two-body interactions (see Chapter 4). The adiabatic compressibility is instead ﬁnite also below Tc and diverges only as T → 0: λ3T 1 ∂n 3 κS = . (3.42) = n ∂P S 5g5/2 (1) kB T In Figure 3.4 we show the equation of state of the ideal Bose gas. The transition line below which the gas exhibits BEC is ﬁxed by the law P v 5/3 = (2π2 m)g5/2 (1)/ 5/3 and is also shown in the ﬁgure. g3/2 (1) In the noninteracting Bose gas we can also easily calculate the oﬀ-diagonal onebody density (2.1), a key quantity for understanding the nature of long-range order. One ﬁnds n(1) (r1 , r2 ) = n ¯ i ϕ∗i (r1 )ϕi (r2 ) (3.43) i

odinger equation (3.9) and n ¯ i are the average where ϕi are the solutions of the Schr¨ occupation numbers (3.14) calculated using the grand canonical ensemble. By comparison with (2.12) we see that the eigenfrequencies and eigenvalues of the one-body

24

The Ideal Bose Gas

P

transition line

T1

T2

vc

v

Figure 3.4 Pressure of the ideal Bose gas as a function of v = V /N for two diﬀerent temperatures. Below vc the pressure is constant. The transition line (dashed curve) is also shown (see text).

density matrix coincide with the solutions of the Schr¨ odinger equation and with the corresponding average occupation numbers. The same property also holds for the ideal Fermi gas and is the consequence of the noninteracting nature of the system. By separating in eqn (3.43) the contribution of the condensate (i = 0) from that of the thermal component (i = 0) and using the plane wave solutions (3.22) for ϕi we ﬁnally obtain the result (s = r1 − r2 ) eip·s/ 1 (3.44) n(1) (s) = n0 + dp (2π)3 eβp2 /2m − 1 for T < Tc , where n0 = N0 /V is the condensate fraction, and eip·s/ 1 (1) n (s) = dp 2 (2π)3 eβ(p /2m−μ ) − 1

(3.45)

for T > Tc . Recalling the relationships between the one-body density matrix and the momentum distribution n(p) discussed in section 2.1, one can immediately identify the momentum distribution of the ideal Bose gas. In the Bose–Einstein condensed phase (T < Tc ) one ﬁnds the result n(p) = N0 δ(p) +

V 1 , (2π)3 eβp2 /2m − 1

(3.46)

while for T > Tc one obtains n(p) =

1 V . (2π)3 eβ(p2 /2m−μ) − 1

(3.47)

The ideal Bose gas in the box

25

The occurrence of the δ function in the momentum distribution for T < Tc is the clear signature of Bose–Einstein condensation. It is interesting to discuss the behaviour of the one-body density matrix n(1) (s) at large distances. This is ﬁxed by the low p behaviour of the momentum distribution. For T < Tc one can use the low-p expansion 1 exp[βp2 /2m]

−1

≈

2mkB T , p2

(3.48)

so that eqn (3.44) is characterized by the 1/s behaviour n(1) (s) → n0 +

1 1 2 3 (2π) λT s

(3.49)

at large s, where λT is the thermal wavelength (3.24). It is worth noticing that the 1/p2 infrared divergency exhibited by the momentum distribution is not peculiar of the ideal Bose gas. In Chapter 16 we will show that this behaviour is a general consequence of Bose–Einstein condensation at ﬁnite temperature, holding also for interacting systems. In order to discuss the behaviour of the one-body density above Tc it is convenient to calculate the Fourier transform (2.8) of the momentum distribution by carrying out ∞ +∞ the integration V n(1) (s) = (4π/s) 0 n(p)p sin(ps/)dp = (2π/s)lm −∞ n(p)peips/ in the complex plane. By moving the contour of integration into the upper half-plane, the integral takes the large s leading contribution from the ﬁrst pole at p = ipc where pc = 2m|μ|. Near the singularity one has n(p) ≈

V 2mkB T , (2π)3 p2 + p2c

(3.50)

and the integral yields the Yukawa-type asymptotic law n(1) (s) ∝

e−pc s/ , s

(3.51)

holding for s /pc . The above results explicitly show that for T > Tc the one-body density goes to zero within a microscopic distance, ﬁxed by the chemical potential, and that only below Tc , due to Bose–Einstein condensation (n0 = 0), does it remain diﬀerent from zero at macroscopic distances. Results (3.44) and (3.45) have been derived imposing cyclic boundary conditions to the solution of the Schr¨ odinger equation. Another choice is to assume that the wavefunctions ϕ vanish at the border of the box (Dirichlet boundary condition). This corresponds to choosing a box with walls of inﬁnite height. The thermodynamic behaviour of a macroscopic system (large N , V ) should not depend on the choice of the boundary conditions, which are expected to modify only the properties at microscopic distances from the boundary. However, the ideal Bose gas is an exception because the shape of the wave function of the condensate is crucially sensitive to the nature of

26

The Ideal Bose Gas 2.5

2

n0(z)

1.5

1

0.5

0

0

0.25

0.5

0.75

1

z/L

Figure 3.5 Density proﬁle n0 (z) = dx dy n0 (r) of a noninteracting condensate conﬁned in a box potential, using periodic (full line) and Dirichlet (dashed line) boundary conditions (see text). The dotted line takes into account the eﬀects of two-body interactions (see Section 11.1).

the boundary. The ground state wave function of the free-particle Hamiltonian p2 /2m, obeying the Dirichlet boundary conditions (namely ϕ = 0 at the boundary), is in fact given by ϕ0 =

πx πy πz 8 sin sin sin , V L L L

(3.52)

with x, y, z deﬁned in the interval [0, L]. Equation (3.52) shows that the condensate contribution N0 | ϕ0 |2 to the density of the gas exhibits a nonuniform behaviour over macroscopic lengths of the order of the size of the system. This diﬀers dramatically from the uniform behaviour obtained by imposing cyclic boundary conditions (see Figure 3.5). The sensitivity of the ideal gas Bose gas model to the choice of the boundary conditions reﬂects its inﬁnite compressibility in the BEC phase. As we will see in Section 11.1 the inclusion of two-body interactions restores the uniformity of the condensate, up to microscopic distances from the boundary.

3.3

Fluctuations and two-body density

In the preceding section we discussed the behaviour of the one-body density (2.1) predicted by the ideal Bose gas model. An interesting feature of the ideal Bose gas is that the one-body density n(1) (r1 , r2 ) also determines the behaviour of the two-body density ˆ † (r)Ψ ˆ † (r )Ψ(r ˆ )Ψ(r). ˆ n(2) (r, r ) = Ψ

(3.53)

Fluctuations and two-body density

27

This can be shown by expanding the ﬁeld operator in terms of the single-particle operators a ˆi (see eqn 2.20) and evaluating the expectation value of the corresponding products of the particle operators: ϕ∗m (r)ϕ∗n (r )ϕ∗k (r )ϕ∗l (r)ˆ a†m a ˆ†n a ˆk a ˆl . (3.54) n(2) (r, r ) = m,n,k,l

Let us ﬁrst consider the ideal Bose gas above Tc . In this case the average values can be safely calculated using the grand canonical ensemble where the diﬀerent eigenstates ϕi (r) are statistically populated in an independent way. Only the terms k = m, l = n and k = n, l = m give a non-vanishing contribution to (3.54), and from expression (3.11) for the grand canonical partition function one ﬁnds the simple relation ˆ ni n ˆk − n ¯in ¯k =

∂2 log Z = δik n ¯ i (¯ ni + 1), ∂(βi )∂(βk )

(3.55)

ˆ†i a ˆi and n ¯ i = ˆ ni is the average occupation number (3.14). It is then poswhere n ˆi = a sible to show that the two-body correlation function takes the form (see, for example, Naraschewski and Glauber, 1999): n(2) (r, r ) = n(r)n(r ) + |n(1) (r, r )|2 ,

(3.56)

where the second term is a quantum-statistical exchange term and we have used result (3.43) for the oﬀ-diagonal one-body density. It manifests a tendency of bosons to cluster together (bunching eﬀect). In the case of fermions this term would have a negative sign, reﬂecting the consequence of the Pauli exclusion principle. For r → r it gives rise to a factor-2 increase in the value of the pair correlation function with respect to the uncorrelated result n2 (r). Below the critical temperature one should proceed more carefully, because the grand canonical ensemble does not provide a correct description of the ﬂuctuations of atoms in the condensate as a consequence of the inﬁnite compressibility of the ideal gas. In this case the ﬂuctuations of atoms in the condensate should not be calculated using eqn (3.55), and one should instead use the result ˆ a†0 a ˆ†0 a ˆ0 a ˆ0 − ˆ a†0 a ˆ0 ˆ a†0 a ˆ0 = O(N ),

(3.57)

consistently with the Bogoliubov prescription discussed in Section 2.2. Below Tc the two-body density then takes the diﬀerent form (see for example, Naraschewski and Glauber, 1998) n(2) (r, r ) = n(r)n(r ) + |n(1) (r, r )|2 − n0 (r)n0 (r ),

(3.58)

where n0 (r) is the density of atoms in the condensate. Equations (3.56–3.58) hold in uniform as well as in nonuniform Bose gases. At T = 0, where n(r) = n0 (r), eqn (3.58) reduces to n(2) (r, r ) = |n(1) (r, r )|2 , revealing perfect second-order coherence.

28

The Ideal Bose Gas

In particular, when r → r one ﬁnds n2 (r, r) = n2 (r), which is a factor 2 less than the corresponding value above Tc . The occurrence of bunching in bosonic gases at ﬁnite temperatures was experimentally observed by Schellekens et al. (2005) who repeated, in atomic gases, the most celebrated Hanbury-Brown and Twiss (1956) experiment with photons, by measuring the two-body correlations of atoms in an expanding cloud above and below the Bose– Einstein condensation threshold. A similar experiment, carried out on a fermionic sample, has pointed out the opposite, anti-bunching eﬀect (Jeltes et al., 2007). Result (3.55) can be used to calculate explicitly the ﬂuctuations of the total number NT = i=0 n ¯ i of atoms out of the condensate, for which one ﬁnds the result Δ(NT2 ) =

n ¯ i (¯ ni + 1).

(3.59)

i=0

In the case of the box potential, for T > Tc , one can safely replace the sum p with the integral (V /(2π)3 ) dp, and eqn (3.59) turns out to be proportional to the volume V of the box. For T ≤ Tc , i.e. in the presence of Bose–Einstein condensation, the situation is diﬀerent. In this case the occupation number of the single-particle states is given by n ¯ p = (exp(βp2 /2m) − 1)−1 and, at small p, the quantity n ¯ p (¯ np + 1) diverges 4 like 1/p . As a consequence, one cannot evaluate the sum (3.59) through the usual replacement p → (V /(2π)3 ) dp. The main contribution to the sum (3.59) is due to the small momenta of order /L ∼ /V 1/3 . This implies that the ﬂuctuations of the thermal component follow the peculiar law Δ(NT2 ) ∝

m2 (kB T )2 V 4/3 , 4

(3.60)

and are hence larger than the values usually found for extensive quantities. Nevertheless, the relative ﬂuctuations Δ(NT2 )/NT2 still tend to zero in the thermodynamic limit, since NT increases linearly with the volume. The peculiar dependence (3.60) exhibited by Δ(NT2 ) is a non-trivial consequence of Bose–Einstein condensation, and is also preserved if one works in the canonical ensemble where both results (3.14) for the average occupation number of the single-particle states and (3.60) for the ﬂuctuations of the thermal component can be exactly derived (Ziﬀ et al., 1977). As already pointed out, the ﬂuctuations of the number of atoms in the condensate cannot be calculated in the grand canonical ensemble, where eqn (3.55) would predict the unphysical and pathological result Δ(N02 ) = N0 (N0 + 1). The value of Δ(N02 ) can instead be safely calculated in the canonical ensemble, where the total number N = N0 + NT does not ﬂuctuate. One consequently obtains the simple result Δ(N02 ) = Δ(NT2 ). Thus in this case the ﬂuctuations of the condensate are governed by the same law (3.60) which hold for the thermal component. In particular they vanish when T → 0. The above results have been derived for the ideal Bose gas. The eﬀects of two-body interactions have been discussed by Giorgini et al. (1998) who have shown that the ﬂuctuations also follow the same law (3.60) in the presence of interactions.

4 Weakly Interacting Bose Gas The ideal Bose gas considered in the previous chapter is a very peculiar system. It is suﬃcient to remember that, in the presence of Bose–Einstein condensation, it has inﬁnite compressibility. Therefore it is not surprising that interactions between particles aﬀect the properties of the gas in a dramatic way, even for very dilute samples. On the other hand, the problem of the almost ideal Bose gas is not trivial since the ground state energy is zero in the absence of interactions and traditional perturbation techniques cannot be applied. This problem was solved by Bogoliubov (1947). The Bogoliubov theory is based on a new perturbation technique and provides the basis of modern approaches to Bose–Einstein condensation in dilute gases. Its description is the main purpose of this chapter.

4.1

Lowest-order approximation: ground state energy and equation of state

Let us discuss some general features of rareﬁed gases. In these systems the following condition holds (diluteness condition): r0 d,

(4.1)

where r0 is the range of the interatomic forces and d = n−1/3 is the average distance between particles, ﬁxed by the density n = N/V of the gas. This condition allows one to consider only conﬁgurations involving pairs of interacting particles, while conﬁgurations with three or more particles interacting simultaneously can be safely neglected. A second important consequence is that the distance between two particles is always large enough to justify the use of the asymptotic expression for the wave function of their relative motion, which is ﬁxed by the scattering amplitude. This implies that all the properties of the system can be expressed in terms of this quantity and that the relevant values of momenta should always satisfy the inequality pr0 / 1. At such momenta the scattering amplitude becomes independent of energy as well as of the scattering angle and can be safely replaced with its low energy value which, according to standard scattering theory, is determined by the s-wave scattering length a (see Section 9.2). In conclusion, one expects that a single parameter, the s wave scattering length a, characterizes all the eﬀects of the interaction on the physical properties of the gas.

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

30

Weakly Interacting Bose Gas

In general, the scattering length can be either small or large compared to the average distance between particles. The gas can be considered weakly interacting if the condition |a| d

(4.2)

is satisﬁed. This is equivalent to requiring the smallness of the so-called gas parameter n|a|3 . A diﬀerent situation can take place in a dilute gas interacting close to a Feshbach resonance, where the inequality (4.1) is still valid, but the condition (4.2) is not in general satisﬁed (see Section 9.2). An important example of a gas interacting with a large value of the scattering length, satisfying the opposite condition |a| d, is provided by the unitary Fermi gas (see Section 16.6). ˆ Let us write the Hamiltonian of the system in terms of the ﬁeld operators Ψ: ˆ = H

2 ˆ † 1 ˆ † (r )Ψ ˆ ˆ † (r)V (r − r)Ψ(r ˆ )Ψ(r)dr ˆ ∇Ψ (r)∇Ψ(r) Ψ dr + dr, 2m 2

(4.3)

where V (r) is the two-body potential and, for the moment, we have not included external ﬁelds. For a uniform gas occupying a volume V the ﬁeld operators can be conveniently written in the form: ˆ Ψ(r) =

p

1 a ˆpi √ eip·r/ , V

(4.4)

where a ˆp is the operator annihilating a particle in the single-particle state with momentum p and the values of p satisfy the usual cyclic boundary conditions. Substitution of (4.4) into (4.3) gives the equivalent expression p2 1 a ˆ†p a ˆp + ˆ†p1 +q a ˆ†p2 −q a ˆp1 a ˆp2 (4.5) Vq a 2m 2V for the Hamiltonian with Vq = V (r) exp[−iq · r/]dr. In real systems the interatomic potential always contains a short-range term, which makes it diﬃcult to obtain the solution of the Schr¨ odinger equation at the microscopic level. In particular, the scattering of slow particles cannot be worked out using perturbation theory. On the other hand, in virtue of the above discussion on the diluteness criterion, we conclude that the actual form of the two-body potential is not important in order to describe the macroscopic properties of the gas, provided the potential gives the correct value of the s-wave scattering length. In order to work out the many-body formalism in the simplest way, it is therefore convenient to replace the microscopic potential V with an eﬀective, soft potential Veff (see Figure 4.1), to which perturbation theory can be safely applied. Since the physical properties must depend uniquely on the value of the scattering length, this procedure will provide the correct answer to the many-body problem as far as the macroscopic properties of the system are concerned. ˆ = H

Lowest-order approximation: ground state energy and equation of state

31

Potential

V

Veff 0

Distance

Figure 4.1 Schematic representation of the interatomic potential V (solid line) and the eﬀective potential Veff . V and Veff yield the same s-wave scattering a. In order to apply Bogoliubov theory the range of both potentials should be much smaller than the average distance n−1/3 .

Since only small momenta are involved in the solution of the many-body problem, we are allowed to consider only the q = 0 value of the Fourier transform of Veff : V0 = Veff (r)dr (4.6) and to write the Hamiltonian in the form: p2 1 ˆ = a ˆ†p a V0 ˆp + ˆ†p2 a ˆp1 a ˆp2 . (4.7) a ˆ†p1 a H 2m 2V The crucial point of the theory now is to use the Bogoliubov prescription, i.e. to replace the operator a ˆ0 with a c-number: a ˆ0 ≡ N0 (4.8) in the Hamiltonian (4.7). This substitution cannot be made for a realistic potential since it would result in a poor approximation at short distances of the order of r0 where the potential is strong and quantum correlations are important. The replacement is instead accurate in the case of a soft potential whose perturbation is small at all distances. In an ideal gas at T = 0 all the atoms are in the condensate and N0 = N . In a dilute gas the occupations numbers for states with p = 0 are ﬁnite but small. This means that, in the ﬁrst approximation, we can neglect in the Hamiltonian (4.7) all the terms containing the operators a ˆp and a ˆ†p with p = 0. Since in the same approximation one √ has N0 ∼ N , one can replace a ˆ0 with N and the ground state energy takes the form E0 =

N 2 V0 . 2V

(4.9)

32

Weakly Interacting Bose Gas

To the same order of approximation one can easily express the parameter V0 of (4.9) in terms of the scattering length a, using the result V0 = 4π2 a/m of the Born approximation. The ground state energy (4.9) can then be rewritten as E0 =

1 N gn , 2

(4.10)

where n = N/V is the density of the gas and we have introduced the relevant interaction coupling constant g=

4π2 a , m

(4.11)

ﬁxed by the s-wave scattering length a. According to the considerations presented in the ﬁrst part of this chapter, results (4.10) and (4.11), which relate the ground state energy to the s-wave scattering length, are valid for arbitrary interactions including the extreme case of hard-sphere potentials. On the contrary, the relation V0 = 4π2 a/m between the scattering length and the parameter V0 holds only if the ﬁrst-order Born approximation is applicable. Equation (4.10) shows that, contrary to the ideal case, the pressure of a weakly interacting Bose gas does not vanish at zero temperature: P =−

∂E0 gn2 = . ∂V 2

(4.12)

Accordingly, the compressibility is also ﬁnite: 1 ∂n = ∂P gn

(4.13)

and tends to inﬁnity when g → 0. Using the hydrodynamic relation 1 ∂n = 2 mc ∂P for the compressibility, one obtains the important expression gn c= m

(4.14)

(4.15)

for the sound velocity. In the next section we will prove that this result for c coincides with the value obtained by starting from the dispersion relation of the elementary excitations in the long wavelength limit. The condition of thermodynamic stability implies that the quantity ∂n/∂P must be positive, i.e. a > 0. We then arrive at the important conclusion that a dilute uniform Bose–Einstein condensed gas can exist only if the value of the s-wave scattering length is positive. In Section 11.6 we will show that, in the presence of external ﬁelds, Bose– Einstein condensed gases can also exist, in a metastable conﬁguration, if the scattering length is negative and suﬃciently small.

Higher-order approximation: excitation spectrum and quantum ﬂuctuations

33

It is ﬁnally important to remark that, unlike the ideal gas, the chemical potential of the interacting gas is not equal to zero, but is given by μ=

∂E0 = gn, ∂N

(4.16)

and is always positive at zero temperature. Using result (4.15) for the sound velocity one can also write the chemical potential of a dilute Bose gas as μ = mc2 .

(4.17)

Result (4.17) holds only for a dilute Bose gas. In general the relation between the chemical potential and the T = 0 sound velocity is given by the formula mc2 = n∂μ/∂n.

4.2

Higher-order approximation: excitation spectrum and quantum ﬂuctuations

Result (4.10) for the ground state energy has been obtained by taking into account in eqn (4.7) only the particle operators a ˆp and a ˆ†p with p = 0. Terms containing only one particle operator with p = 0 do not enter the Hamiltonian (4.7) because of momentum conservation. By retaining all the quadratic terms in the particle operators with p = 0, one obtains the following decomposition of the Hamiltonian: p2 V0 † † ˆ = V0 a H ˆ†0 a a ˆ†p a ˆ†0 a ˆ0 a ˆ0 + ˆp + (4ˆ a0 a ˆp a ˆ0 a ˆp + a ˆ†p a ˆ†−p a ˆ0 a ˆ0 + a ˆ†0 a ˆ†0 a ˆp a ˆ−p ). 2V 2m 2V p=0

(4.18) √ As we have done previously, we can replace a ˆ†0 and a ˆ0 with N in the third term of eqn (4.18). However, in the ﬁrst term one has to work with higher accuracy by using the normalization relation a ˆ†0 a ˆ0 + p=0 a ˆ†p a ˆp = N or, neglecting higher-order terms, a ˆ†0 a ˆ†0 a ˆ0 a ˆ0 = N 2 − 2N

a ˆ†p a ˆp .

(4.19)

p=0

An analogous situation takes place when one looks for the relation between V0 and the scattering length a, beyond the lowest-order Born approximation. In this case one has to calculate a up to quadratic terms in V0 . Using higher-order perturbation theory one ﬁnds the result (see, for example, Landau and Lifshitz, 1987b): ⎛ ⎞ 2 m ⎝ m⎠ V a= V0 − 0 (4.20) 4π2 V p2 p=0

or, with equivalent accuracy, ⎞ m g ⎠, V0 = g ⎝1 + V p2 ⎛

p=0

(4.21)

34

Weakly Interacting Bose Gas

where g is related to the scattering length by eqn (4.11). Equation (4.21) renormalizes the relationship between the eﬀective potential and the physical coupling constant g. The divergency occurring for large p in the sum of eqn (4.21) is the consequence of the replacement of the matrix element Vq with the constant value V0 . This term is crucial to ensure a convergent result for the ground state energy calculated to the higher order of approximation (see eqn (4.30) below). Substitution of eqns (4.19) and (4.21) into (4.18) yields the following expression for the Hamiltonian: N 2 p2 † 1 mgn † † † ˆ H=g + a ˆ a 2ˆ ap a ˆp + gn ˆp + a ˆp a ˆ−p + a ˆp a ˆ−p + 2 , (4.22) 2V 2m p 2 p p=0

which turns out to be uniquely ﬁxed by the interaction coupling constant g. The Hamiltonian (4.22) is quadratic in the operators a ˆp , a ˆ†p and can be diagonalized by the linear transformation ∗ ˆ† a ˆp = upˆbp + v−p ˆ†p = u∗pˆb†p + v−pˆb−p , b−p , a

(4.23)

known as the Bogoliubov transformation. This transformation introduces a new set of operators, ˆbp and ˆb†p , to which we impose the same Bose commutation relations ˆbpˆb† − ˆb† ˆbp = δpp obeyed by the original particle operators a ˆp and a ˆ†p . It is easy to p p check that the commutation relations are satisﬁed if |up |2 − |v−p |2 = 1,

(4.24)

up = cosh αp , v−p = sinh αp .

(4.25)

i.e. if one can write

The parameter αp will be chosen in order to make the coeﬃcient of the non-diagonal terms b†p b†−p and bp b−p in the Hamiltonian (4.22) vanish. This condition takes the form 2 gn p 2 2 (|up | + |v−p | ) + + gn up v−p = 0. (4.26) 2 2m Using the properties cosh 2α = cosh2 α + sinh2 α and sinh 2α = 2 cosh α sinh α, one immediately ﬁnds that eqn (4.26) is solved by the choice coth 2αp = −

p2 /2m + gn gn

(4.27)

and that the explicit form of the coeﬃcients up and vp becomes up , v−p = ±

p2 /2m + gn 1 ± 2(p) 2

1/2 ,

(4.28)

Higher-order approximation: excitation spectrum and quantum ﬂuctuations

35

with (p) deﬁned by eqn (4.31) below. By virtue of the Bogoliubov transformation (4.23) and of result (4.28) for up and v−p , the Hamiltonian (4.22) can ﬁnally be reduced to the diagonal form ˆ = E0 + H (p)ˆb†pˆbp , (4.29) where E0 = g

1 m(gn)2 p2 N2 + + (p) − gn − 2V 2 2m p2

(4.30)

p=0

is the ground state energy calculated to the higher order of approximation and

gn 2 p + (p) = m

p2 2m

2 1/2 (4.31)

is the famous Bogoliubov dispersion law for the elementary excitations of the system (Bogoliubov, 1947). Results (4.29)–(4.31) have a deep physical meaning. They show that the original system of interacting particles can be described in terms of a Hamiltonian of independent quasi-particles having energy (p) and whose annihilation and creation operators are given, respectively, by ˆbp and ˆb†p . The ground state of the interacting system then corresponds to the vacuum of quasi-particles: ˆbp |vac = 0

(4.32)

for any p = 0. The ground state energy (4.30) can easily be calculated by replacing the sum with an integral in momentum space. The result is (Lee and Yang, 1957; Lee et al., 1957)

128 N2 3 1/2 E0 = g 1 + √ (na ) , (4.33) 2V 15 π while the chemical potential μ = ∂E0 /∂N is given by

32 3 1/2 μ = gn 1 + √ na . 3 π

(4.34)

It is not diﬃcult to see that in the integration yielding the above results only values √ p ∼ mgn = mc are important. For such momenta the parameter pa/ ∼ (na3 )1/2 is very small compared to unity, which is consistent with our initial assumptions. This justiﬁes a posteriori the replacement of Vq with V0 made in the calculation of the renormalized scattering length (4.20). It is also worth pointing out that the perturbation parameter of the expansion (4.33) is given by (na3 )1/2 . One can show that the next term in the expansion is proportional to (na3 ) ln(na3 ). The coeﬃcient in front of the logarithm can also be calculated with proper accuracy. The one inside the logarithm depends instead on the details of the interaction (Wu, 1959).

36

Weakly Interacting Bose Gas

The Lee–Huang–Yang (LHY) expansion (4.33)–(4.34) can also be formulated in the form P (μ, a) =

2 h(ν), ma5

(4.35)

with ν = μa3 /g = μma2 /(4π2 ) and 128 √ h(ν) = 2πν 2 1 − √ ν , 15 π

(4.36)

exploiting the dependence of the pressure of the Bose gas on the scattering length and on the chemical potential. In this form the equation of state is well suited for a direct comparison with the experimental data available in trapped atomic gases. The ﬁrst term in eqn (4.36) corresponds to the mean ﬁeld result predicted by Bogoliubov theory, while the second one is the LHY correction. The procedure to obtain experimentally the equation of state of uniform matter starting from the density proﬁles of trapped atomic gases will be discussed in Section 13.6). In Figure 4.2 we report the experimental results obtained by Navon et al. (2011), obtained at the lowest available temperatures, which compare fairly well with theory, pointing out in a quantitative way the role played by beyond-mean-ﬁeld eﬀects in the equation of state of a dilute Bose–Einstein condensed gas.

h(ν ) [10–5]

5 4 3 2 1 0 0

1

2 ν = μ a3/g [10–3]

3

Figure 4.2 Experimental equation of state (EoS) of the homogeneous Bose gas expressed as the normalized pressure h as a function of the gas parameter ν (see text). The solid line corresponds to the LHY prediction, and the dashed line to the mean-ﬁeld EoS h(ν) = 2πν 2 . The prediction of the Quantum Monte Carlo EoS, obtained at T /Tc = 0.25, is almost indistinguishable from the LHY EoS. From Navon et al. (2011). Reprinted with permission c 2011, American Physical Society. from Physical Review Letters, 107, 135301;

Particles and elementary excitations

37

We have often referred to (4.10) or (4.33) as the ground state energy of the interacting many-body system. This statement is not, however, completely correct. It is, in fact, well known that the ground state of most physical systems interacting with interatomic potentials does not correspond to a gas, but rather to a solid. For such systems the gas phase in the quantum degenerate regime actually represents only a metastable conﬁguration where thermalization is ensured by two-body collisions. The Bogoliubov theory discussed above provides a description of this metastable phase. The theory ignores three-body collisions which, in actual systems, will eventually drive the system into the solid conﬁguration. Experiments carried out on several atomic species have not only proven that the quantum gas phase can be realized, but that it survives for times large enough to allow for systematic measurements of many relevant physical quantities. With this caveat in mind we will refer in the following to (4.32) and (4.33) as the ground state and ground state energy of the system respectively.

4.3

Particles and elementary excitations

In the preceding section we have shown that the excited states of an interacting Bose gas can be described in terms of a gas of noninteracting quasi-particles (see eqn (4.29)). For small momenta p mc the dispersion law (4.31) of quasi-particles takes the phonon-like form (p) = cp.

(4.37)

where c = gn/m is the sound velocity which coincides with the result (4.15) derived starting from the equation of state (4.12). The Bogoliubov theory then predicts that the long-wavelength excitations of an interacting Bose gas are sound waves. These excitations can be also regarded as the Goldstone modes associated with breaking of gauge symmetry caused by Bose–Einstein condensation. It is also worth noticing that in the phonon regime the coeﬃcients (4.28), characterizing the Bogoliubov transformation (4.23), exhibit a divergent infrared behaviour: up → −v−p → (mc/2p)1/2 . This reﬂects the fact that in the phonon regime the Bogoliubov transformation introduces a drastic modiﬁcation in the nature of elementary excitations with respect to the ideal gas. In the opposite limit p mc the dispersion law approaches the free particle law: (p) ≈

p2 + gn. 2m

(4.38)

Correspondingly, one has |v−p | up ∼ 1 and ap ∼ bp . The transition between the phonon and particle regimes takes place when p2 /2m ∼ gn = mc2 , i.e. for p ∼ mc (see Figure 4.3). By setting p2 /2m = gn with p = /ξ one can deﬁne the characteristic interaction length ξ=

2 1 =√ , 2mgn 2 mc

(4.39)

38

Weakly Interacting Bose Gas 30

p2/2m + mc 2

ε( p)

20

10

p2/2m cp

0

ħ/ξ

p

Figure 4.3 Bogoliubov dispersion of elementary excitations (see eqn (4.31) with gn = mc2 ). The transition between the phonon (cp) and the free particle (p2 /2m) regimes takes place at p ∼ /ξ. Energy is given in units of mc2 .

also called the healing length. The physical meaning of this quantity will be discussed in Chapter 5. The thermodynamic behaviour of a gas of independent excitations (quasi-particles) can easily be obtained, starting from the results derived in Section 3.1 for the ideal gas, by simply setting the chemical potential equal to zero and using the expression (4.31) for the energy of the elementary excitations. This assumption is correct at low temperatures where the elementary excitations do not interact with each other and one can safely use the Bogoliubov dispersion law (4.31). The average occupation number Np of quasi-particles carrying momentum p is given by (see eqn (3.14)) Np ≡ ˆb†pˆbp =

1 . exp[β(p)] − 1

(4.40)

This should not be confused with the average particle occupation number ˆ a†p a ˆp (see eqn (4.43) below). In this connection it is worth noticing that the chemical potential of the gas of quasi-particles is zero by deﬁnition, since their number is not ﬁxed but is determined by the condition of thermodynamic equilibrium, in analogy with the Planck’s law of black body radiation. By setting μ = 0 in the eqns (3.15)–(3.16) we can also evaluate the free energy A = E − T S associated with the gas of quasi-particles. One ﬁnds A(T, V ) = E0 + kB T V

ln 1 − e−β(p)

dp , (2π)3

(4.41)

Particles and elementary excitations

39

where we have added the energy E0 of the system evaluated at zero temperature (ground state energy). Notice that the thermal contribution to A is aﬀected by two-body interactions through the dependence of (p) on the interaction coupling constant g (see eqn (4.31)). The low T expansion of eqn (4.41) yields the result 4

A = E0 − V

π 2 (kB T ) , 903 c3

(4.42)

holding for kB T mc2 . Equation (4.42) reproduces the characteristic T 3 law for the speciﬁc heat in the phonon regime. This diﬀers from the prediction of the ideal gas where the speciﬁc heat behaves like T 3/2 . As already mentioned it is important to distinguish between the quasi-particle occupation number ˆb†pˆbp given by (4.40) and the particle occupation number ˆ a†p a ˆp already introduced in Section 2.2 and directly related to the particle momentum distribution. This can easily be calculated by using the Bogoliubov transformation (4.23) in order to express the operator a ˆ†p a ˆp in terms of the operators ˆb and ˆb† . Since the averages ˆbpˆb−p and ˆb†pˆb†−p identically vanish, one easily obtains the useful relationship np = ˆ a†p a ˆp = |v−p |2 + |up |2 ˆb†pˆbp + |v−p |2 ˆb†−pˆb−p ,

(4.43)

holding for p = 0. The number of atoms in the condensate can be calculated through the relation

V |up |2 + |v−p |2 2 , (4.44) N0 = N − dp |v np = N − | + p (2π)3 exp[β(p)] − 1 p=0

where we have used result (4.40) for ˆb†pˆbp . The interactions in the gas cause the presence of particles with non-zero momentum even at absolute zero where ˆb†pˆbp = 0. This is the consequence of quantum ﬂuctuations, accounted for by the ﬁrst term in the right-hand side of eqn (4.43). Using result (4.28) for v−p , one ﬁnds that the particle occupation number is given, at T = 0, by np =

1 p2 /2m + mc2 − . 2(p) 2

(4.45)

Equation (4.45) exhibits a singular behaviour at small momenta: (np )p→0 =

mc . 2p

(4.46)

In Section 7.4 we will show that this infrared divergence is not a peculiarity of dilute Bose gases, but is a general property exhibited by Bose–Einstein condensed systems at zero temperature. At high momenta one instead ﬁnds the asymptotic behaviour (np )p→∞ =

m2 c2 , p4

(4.47)

40

Weakly Interacting Bose Gas

holding for p mc. A simple result is also found for the so-called anomalous particle distribution n ˜ p = ˆ a†p a ˆ†−p for which one ﬁnds the result n ˜ p = mc2 /2(p). Integration of (4.44) at T = 0 yields the result

1/2 8 N0 n0 ≡ = n 1 − √ na3 (4.48) V 3 π for the condensate density, revealing that the quantum depletion of the condensate is √ ﬁxed by the same parameter na3 characterizing the ﬁrst corrections to the ground state energy (see eqn (4.33)). Diﬀerently from the LHY expansion (4.33) for the energy, the ﬁrst correction to the condensate fraction does not require the renormalization of the scattering length. This is due to the fact that, to lowest order, the value of n0 does not depend on a being equal to the total density n. It is also worth mentioning that the integral dp | v−p |2 is exhausted by momenta up to p ∼ mc, which is consistent with the applicability of Bogoliubov theory. The convergence of result (4.48) at large momenta is ensured by the fact that the particle momentum distribution (4.45) behaves as 1/p4 for large momenta (see eqn (4.47)). The convergence is, however, very slow, and one needs to integrate up to p ∼ 10mc in order to saturate 90 per cent of the integral. Because of the 1/p4 behaviour of np , the kinetic energy KE =

p2 np 2m p

(4.49)

exhibits an ultraviolet divergence, showing that this quantity cannot be calculated starting from the Bogoliubov prediction for the particle momentum distribution and is sensitive to the inclusion of dynamic correlations at a more microscopic scale. The actual value of the kinetic energy at T = 0 can be expressed in terms of the dependence of the scattering length a on the atomic mass. Indeed, from the exact identity KE = m−1 ∂E0 /∂m−1 , where E0 = 0|H|0 is the ground state energy, and using result (4.10) for E0 , one ﬁnds the nontrivial identity (Cherny and Shanenko, 2000) KE = 2π

∂(am−1 ) 2 Nn . m ∂m−1

(4.50)

In the case of a gas interacting with a hard-sphere potential, where a is independent of m, eqn (4.50) directly shows that the kinetic energy coincides with the total energy E0 . It is also worth noticing that, diﬀerently from the calculation of the kinetic energy, no ultraviolet divergence is encountered in the sum (4.30) for the total (kinetic plus interaction) energy which is safely evaluated within the Bogoliubov approach (see eqn (4.33)). Starting from the T = 0 result (4.45) one can calculate the one-body density matrix (see Chapter 2). Using eqn (2.8) and the relationship (2.17) between the momentum distribution n(p) and the particle occupation number np , one obtains the result 1 1 n(1) (s) = n0 + dp | v−p |2 eip·s/ = n0 + 3 D(s/ξ), (4.51) (2π)3 ξ

Particles and elementary excitations

41

where ξ is the healing length (4.39), and we have deﬁned the dimensionless function 1 + k2 1 1 √ D(˜ s) = dk − 1 ei˜s·k (4.52) 2 (2π)3 k 4 + 2k 2 having set k = pξ/ with ˜s = s/ξ. For large s˜ the function D(˜ s) behaves like √ √ ( 32π 2 s˜2 )−1 , while for s˜ → 0 it approaches the constant value (3 8π 2 )−1 . Equation (4.51) shows that ξ is the relevant length characterizing the behaviour of the one-body density matrix of a dilute gas at zero temperature. Equation (4.43) also accounts, through the terms ˆb†ˆb, for the contribution of the thermal excitations to np . In the low-energy regime where kB T , the occupation number of the excitations follows the law ˆb†pˆbp kT /(p), as clearly emerges from (4.40). On the other hand, from eqn (4.28), one ﬁnds, in the phonon regime, |up |2 + |v−p |2 → mc2 /(p) so that at ﬁnite temperatures the particle distribution function exhibits the divergent behaviour np →

mkT mkT mc2 = , 2 (p) p2

(4.53)

which is stronger than the one occurring at zero temperature (see eqn (4.46)). The infrared divergence (4.53) is equal, apart from a factor 2, to the one exhibited by the ideal Bose gas at ﬁnite temperatures (see eqn (3.48)). By integrating the term containing the Bose factor in eqn (4.44), one can calculate the temperature dependence of the condensate which, for temperatures satisfying the inequality kT mc2 , takes the form m(kB T )2 n0 (T ) − n0 (T = 0) =− . n0 (T = 0) 12nc3

(4.54)

Let us ﬁnally comment on the range of applicability of the theory presented above. The fundamental assumption is that the majority of atoms are in the condensate, i.e. N0 ≈ N . This means, in particular, that the correction (4.54) must be small. This result is obvious at low enough temperatures. However the depletion of the condensate is also small at temperatures of the order of the chemical potential where one obtains δn0 /n0 ∼ (na3 )1/2 1. At higher temperatures the elementary excitations which mainly contribute to the depletion satisfy the condition (p) mc2 and hence correspond to free particles. As a consequence, in this regime the temperature dependence of n0 (T ) approaches the form given by the ideal gas. On the other hand, in a dilute gas the condition mc2 kB Tc , where Tc is the critical temperature (2.28), must be always satisﬁed, being exactly equivalent to the diluteness condition (4.2). One then concludes that, provided the condition T Tc0

(4.55)

is satisﬁed, both the ‘phonon’ kB T mc2 regime and the ‘particle’ regime kB T mc2 are compatible with the use of the Bogoliubov approach. An example of application of the Bogoliubov approach concerns the mechanism of hybridization between ﬁrst and second sound in a dilute Bose gas, which takes place at temperatures of order kB T ∼ mc2 (see Section 6.6).

5 Nonuniform Bose Gases at Zero Temperature In this chapter we develop the theory of nonuniform dilute Bose gases. The problem is important for at least two reasons. On one hand, Bose–Einstein condensation in atomic gases was experimentally achieved in traps, where gases are naturally nonuniform. On the other hand, nonuniformity gives rise to a new series of phenomena where the quantum nature of the system appears in a peculiar way. The theory can be developed for both stationary and nonstationary situations and hence permits the investigation of a wide class of physical problems. The formalism developed in this chapter will be extensively employed in the second part of this volume to discuss various situations of experimental interest.

5.1

The Gross–Pitaevskii equation

In order to study interacting nonuniform gases one must generalize the Bogoliubov theory introduced in the previous chapter. To this purpose we will use the Bogoliubov prescription for the ﬁeld operator in its general form (2.20). This implies that, to the lowest-order approximation and at very low temperature, one can simply replace ˆ t) with a classical ﬁeld Ψ(r, t), also called the order parameter or the the operator Ψ(r, wave function of the condensate. This procedure has indeed a deep physical meaning. In fact the replacement is analogous to the transition from quantum electrodynamics to the classical description of electromagnetism. We know that this is justiﬁed if one has a large number of photons in the same quantum state. In this case the noncommutativity of the ﬁeld operators is not important and one can describe the electromagnetic ﬁeld employing classical functions, i.e. the electric and the magnetic ﬁelds, which obey the Maxwell equations. In our case the presence of a large number of atoms in a single state (Bose–Einstein condensate) permits the introduction of the classical function Ψ(r, t). However, we have not yet established the equation governing this ﬁeld. For this purpose ˆ t), in the Heisenberg representation, fulﬁls we remember that the ﬁeld operator Ψ(r, the exact equation i

2 2 ∂ ˆ ˆ t), H] ˆ = − ∇ + Vext (r, t) Ψ(r, t) = [Ψ(r, ∂t 2m ˆ t), ˆ , t)dr Ψ(r, ˆ † (r , t)V (r − r)Ψ(r + Ψ

(5.1)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

The Gross–Pitaevskii equation

43

ˆ and the which can be obtained using expression (4.3) for the Hamiltonian H commutation relations (2.2) for the ﬁeld operator. We can now follow the same considerations used in Chapter 4. It would be wrong ˆ t) with Ψ(r, t) for a realistic potential. The replacement is, however, to replace Ψ(r, accurate if one uses an eﬀective soft potential Vef f where Born approximation is applicable. The potential Vef f should reproduce the same low-energy scattering properties given by the bare potential V . By assuming that the function Ψ(r, t) varies slowly on distances of the order of the range of the interatomic force, one can substitute r with r in the arguments of Ψ to ﬁnally obtain the equation 2 2 ∇ ∂ 2 + Vext (r, t) + g|Ψ(r, t)| Ψ(r, t) (5.2) i Ψ(r, t) = − ∂t 2m for the order parameter with g = Vef f (r)dr. By expressing this integral in terms of the s-wave scattering length a, one again recovers the relation (4.11) g=

4π2 a . m

(5.3)

As explained in Chapter 4, the validity of equations (5.2) and (5.3) is not restricted to soft potentials, but holds in general for arbitrary forces, the s-wave scattering amplitude a providing the relevant interaction parameter. Equation (5.2) was derived independently by Gross (1961) and Pitaevskii (1961) and is the main theoretical tool for investigating nonuniform dilute Bose gases at low temperature. It has the typical form of a mean ﬁeld equation where the order parameter must be calculated in a self-consistent way. We have already anticipated that equation (5.2) for the order parameter Ψ plays a role analogous to the Maxwell equations in classical electrodynamics. One can say that the condensate wave function represents the classical limit of the de Broglie wave, where the corpuscular aspect of matter is no longer important. Still, unlike the Maxwell equations, eqn (5.2) contains the quantum constant explicitly. The reason for this diﬀerence is due to the diﬀerent relation between energy () and momentum (p) in the case of photons and atoms, which implies a diﬀerent relation between the frequency ω = / and the wave vector k = p/ of the corresponding waves. For photons, the relation = cp provides the classical dispersion relation ω = ck. For atoms, the relation = p2 /2m instead yields the dispersion law ω = k 2 /2m, containing explicitly . This implies, in particular, that the coherence phenomena, like interference, depend on the value of the Planck constant (see Chapter 15). Another important peculiarity of the Gross-Pitaevskii eqn (5.2) is its nonlinearity. This arises from the interaction among particles and introduces an important analogy between Bose–Einstein condensation in atomic gases and nonlinear optics. Coherence and interaction eﬀects are important features which can be investigated starting from the Gross-Pitaevskii equation and which make the physics of Bose–Einstein condensation a rich ﬁeld of experimental and theoretical research. Let us brieﬂy discuss the conditions of applicability of eqn (5.2). First, the total number of atoms should be large enough because only in this case are we authorized

44

Nonuniform Bose Gases at Zero Temperature

to use the concept of Bose–Einstein condensation. Second, in order to replace the ﬁeld operator with the classical ﬁeld we must assume that the condition (4.3) of weak interactions is satisﬁed and that the temperature of the sample is low enough. This permits us to ignore both the quantum and the thermal depletion of the condensate and implies that the order parameter is normalized to the total number of atoms: |Ψ|2 dr = N . The same conditions were also required to derive the Bogoliubov theory of weakly interacting Bose gases to lowest order (see Section 4.1) and imply that the density of the condensate coincides with the density of the gas: n(r) = |Ψ(r)|2 .

(5.4)

A further condition is that we are only allowed to use the Gross-Pitaevskii eqn (5.2) to investigate phenomena taking place over distances much larger than the scattering length. In fact, for microscopic distances the approximations needed to derive (5.2) are no longer valid. It is not diﬃcult to build the many-body wave function corresponding to a given solution Ψa of the Gross-Pitaevskii equation. In fact, as a consequence of the diluteness of the gas, one can ignore, to ﬁrst approximation, correlations among particles, and write the many-body wave function of the system in the factorized form (Hartree–Fock approximation) 1 1 1 √ Ψa (r2 ) . . . √ Ψa (rN ) , Φa (r1 , r2 , . . . rN ) = √ Ψa (r1 ) (5.5) N N N where Ψa is the order parameter obtained by solving the Gross-Pitaevskii equation. Since the Gross-Pitaevskii equation is not linear, two solutions, Ψa and Ψb , corresponding to diﬀerent values μa and μb of the chemical potential, are not necessarily orthogonal, i.e. the quantity N −1 drΨ∗a Ψb can be diﬀerent from zero. At ﬁrst sight this seems to contradict the orthogonality condition predicted by quantum mechanics. However, one should not confuse the order parameter with the many-body wave function. The nonlinearity of the GP equation for the order parameter follows directly from the nonlinearity of eqn (5.1) for the ﬁeld operator. Actually, equation (5.5) permits us to easily understand why the nonlinearity of the GP equation is compatible with the orthogonality of the corresponding many-body wave functions. In fact, even if two solutions of the GP equation are not orthogonal, the corresponding many-body wave functions (5.5) become orthogonal in the thermodynamic limit, their scalar product being given by the expression (Φa , Φb ) = (N−1 drΨ∗a Ψb )N . This quantity tends to zero when N → ∞, since the integral N −1 drΨ∗a Ψb is always smaller than unity, except when Ψa ≡ Ψb . This result also conﬁrms that the consistency of the mean ﬁeld picture, expressed by the Gross-Pitaevskii equation, is only guaranteed for large values of N . An alternative way to derive the time-dependent eqn (5.2) is obtained by imposing the stationarity condition ∂ δ −i Ψ∗ Ψ drdt + Edt = 0 (5.6) ∂t

The Gross–Pitaevskii equation

45

to the action, yielding the equation i

δE ∂Ψ(r, t) = ∂t δΨ∗ (r, t)

for the order parameter, where 2 g 4 2 2 |∇Ψ| + Vext (r)|Ψ| + |Ψ| dr E= 2m 2

(5.7)

(5.8)

is the energy functional of the system. Let us discuss the conservation laws associated with eqn (5.2). First of all, this equation guarantees the conservation of the number of atoms N = |Ψ|2 dr. Let us multiply (5.2) by Ψ∗ and subtract the complex conjugate of the resulting expression. One then easily obtains the continuity equation ∂n + divj = 0, ∂t

(5.9)

where we have used eqn (5.4) for the density of the gas, and introduced the current density j(r, t) = −

i (Ψ∗ ∇Ψ − Ψ∇Ψ∗ )) = n ∇S. 2m m

Here S is the phase of the order parameter, deﬁned by Ψ(r, t) = n(r, t)eiS(r,t) .

(5.10)

(5.11)

From eqn (5.9) it immediately follows that dN/dt = 0. Equation (5.10) shows that the vector vs (r, t) =

∇S(r, t) m

(5.12)

is the velocity of the condensate ﬂow which turns out to be irrotational (curlvs = 0), a typical characteristic of superﬂuids, as we will discuss in Chapter 6. From eqn (5.2) it also follows that the energy (5.8) of the system is conserved, i.e. dE/dt = 0. This can easily be checked by direct diﬀerentiation of (5.8) and use of the Gross-Pitaevskii eqn (5.2). Of course this result holds only if the external potential does not depend on time. Finally, the equation for the momentum density of the gas can be written in the form m where Πik =

∂ji ∂Πik ∂Vext + = −n , ∂t ∂xk ∂xi

2 ∂Ψ ∂Ψ∗ ∂ 2 Ψ∗ gn2 δik , − Ψ + c.c. + 2 4m ∂xi ∂xk ∂xi ∂xk 2

(5.13)

(5.14)

46

Nonuniform Bose Gases at Zero Temperature

is the momentum ﬂux tensor. Equation (5.13) explicitly shows that, in the absence of external ﬁelds, the total momentum p = m jdr is also conserved. It is also useful to derive an explicit equation for the phase S of the order parameter. Inserting (5.11) into (5.2) one ﬁnds the equation √ ∂ 1 2 √ ∇2 n = 0 . S+ mv2s + Vext + gn − (5.15) ∂t 2 2m n It is worth pointing out that the equation of continuity (5.9) and the equation for the phase (5.15) provide a closed set of coupled equations, exactly equivalent to the original Gross-Pitaevskii equation. The Planck constant enters the right-hand side of (5.15) through the term containing the gradient of the density. This is called the ‘quantum pressure’ term and reveals that the importance of quantum eﬀects is emphasized in nonuniform gases. The Gross-Pitaevskii eqn (5.2) takes a simple form in the case of stationary solutions where the condensate wave function evolves in time according to the law (see eqn (2.22)) iμt Ψ (r, t) = Ψ0 (r) exp − . (5.16) The time dependence is ﬁxed by the chemical potential ∂E , ∂N while the Gross-Pitaevskii equation reduces to 2 2 ∇ − + Vext (r) + g|Ψ0 (r)|2 − μ Ψ0 (r) = 0, 2m μ=

(5.17)

(5.18)

where we have assumed that the external potential does not depend on time. The value of the chemical potential μ is ﬁxed by the normalization condition |Ψ0 (r)|2 dr = N . A mathematically rigorous proof that eqn (5.18) describes the ground state of a dilute Bose gas of particles interacting with repulsive forces has been given by Lieb et al. (2000). A rigorous derivation of the time-dependent GP eqn (5.2) has been given by Erd˝ os et al. (2010). Equation (5.18) can be also obtained by imposing the stationarity condition to the energy (5.8) with respect to variations of Ψ∗0 , with the constraint that the number N of atoms is ﬁxed. This corresponds to using the grand canonical energy E = E − μ |Ψ0 (r)|2 dr (5.19) instead of E in the variational calculation. In this case the natural thermodynamic variable is the chemical potential rather than thenumber of particles, which can be determined using the relation N = − (∂E /∂μ) = |Ψ0 (r)|2 dr. Equation (5.18) admits diﬀerent solutions. The solution with the lowest energy deﬁnes the order parameter of the ground state and in general turns out to be a real

Thomas–Fermi limit

47

function. The excited solutions are instead usually given by complex functions, the vortex state being the most famous example. The Gross-Pitaevskii eqn (5.18) will be systematically employed in the second part of this volume to calculate the wave function of the condensate of interacting Bose gases conﬁned in traps. An equation of similar form has also been considered in connection with the theory of superﬂuidity near the λ point (Ginzburg and Pitaevskii, 1958) where, however, the coeﬃcients of the equation have a diﬀerent meaning. For a uniform gas, in the absence of the external potential, eqn (5.18) simply gives μ = g|Ψ0 |2 = gn in agreement with (4.16). In the same limit eqn (5.8) coincides with the Bogoliubov expression (4.10) for ground state energy. We then conclude that the theory presented in this section, when applied to the ground state, corresponds to the lowest-order approximation of Bogoliubov theory developed in Chapter 4 in the case of uniform gases.

5.2

Thomas–Fermi limit

If the density of the gas changes slowly in space, then the quantum pressure term proportional to 2 in eqn (5.15) can be neglected and the equations of motion simplify further. Let us indicate with D the typical distance characterizing the density variations taking place in the system. This can be the size of the condensate if we are interested in the ground state, or the wavelength of the density oscillations if we √consider time-dependent conﬁgurations. The quantum pressure term scales as √ ∇2 n/ n ∼ D−2 and, according √ to eqn (5.15), becomes negligible if D is much larger than the healing length ξ = / 2mgn introduced in Chapter 4 (see eqn (4.39)) to discuss the transition between the phonon and single-particle regimes in the Bogoliubov excitation spectrum. It is interesting to compare the healing length with the average distance d = n−1/3 between particles. The ratio 1 ξ 1 =√ 3 d 8π (na )1/6

(5.20)

increases by decreasing the value of the gas parameter. However, its dependence on the quantity na3 is very weak. If we neglect the quantum pressure term in eqn (5.15) (Thomas–Fermi approximation) we ﬁnd the following equation for the gradient of the phase: ∂ 1 m vs + ∇ mv2s + Vext + gn = 0. (5.21) ∂t 2 Notice that in eqn (5.21) the Planck constant has disappeared. Actually this equation coincides with the classical Euler’s equation for potential ﬂow of a non-viscous gas with pressure P = gn2 /2. The sound velocity of such a gas is c = gn/m, in agreement with the Bogoliubov result (4.15). On the other hand, the equation of continuity (5.9) can be rewritten in terms of the superﬂuid velocity vs as ∂n + div(vs n) = 0. ∂t

(5.22)

48

Nonuniform Bose Gases at Zero Temperature

Equations (5.21) and (5.22) have the typical form of the hydrodynamic equations of superﬂuids (see Chapter 6) and will be used extensively in this volume. In the Thomas–Fermi limit the ground state conﬁguration takes a particularly simple form. In fact, using eqn (5.21) with vs = 0 or, equivalently, neglecting the kinetic energy term in (5.18), one obtains the result gn(r) + Vext (r) = μ,

(5.23)

where μ is the ground state chemical potential. Equation (5.23) expresses the condition of local equilibrium for a system whose chemical potential, in the absence of the external ﬁeld, would be given by the Bogoliubov relation μ = gn.

5.3

Vortex line in the weakly interacting Bose gas

As already anticipated, the stationary solutions of the Gross-Pitaevskii equation are characterized by an order parameter varying in time through a global phase ﬁxed by the chemical potential (see eqn (5.16)), and the equation for the order parameter takes the form (5.18). The vortical solution of the GP equation, which will be discussed in the present section, exhibits nontrivial features due to the occurrence of a core region where the density goes to zero. The size of this region turns out to be of the order of the healing length so that the vortex solution cannot be described using the hydrodynamic equations developed in the previous section, but should be found including the quantum pressure term explicitly. Vortices are not, in general, stable conﬁgurations and only in a frame rotating at high angular velocity do they correspond to local or global minima of the energy functional (5.8). Quantized vortex lines were predicted by Onsager (1949) and Feynman (1955). The theory presented in this section was developed by Gross (1961) and Pitaevskii (1961). The study of vortices provides an important insight into the problem of rotations, a subject of great relevance in the physics of superﬂuids. In fact, it is well known that a superﬂuid cannot rotate as a normal ﬂuid. In usual systems the velocity ﬁeld corresponding to a rotation is given by the rigid-body form: v = Ω × r and is characterized by a diﬀused vorticity: curlv = 2Ω = 0. This velocity ﬁeld contradicts the irrotationality condition (5.12) of superﬂuids, which are consequently expected to rotate in a diﬀerent way. Let us take a gas conﬁned in a macroscopical cylindrical vessel of radius R and length L and let us look for a solution of the Gross-Pitaevskii equation corresponding to a rotation around the axis of the cylinder. Such a solution can be found in the form (see eqn (5.11)) Ψ0 (r ) = eisϕ |Ψ0 (r)|,

(5.24)

√ where we have introduced the cylindrical coordinates r, ϕ, and z and |Ψ0 | = n. Due to the symmetry of the problem the modulus of the order parameter depends only on the radial variable r. The parameter s is an integer in order to ensure that the wave function (5.24) is single valued. This wave function is an eigenstate of the angular momentum with z = s so that the vortex carries a total angular momentum equal

Vortex line in the weakly interacting Bose gas

49

to Lz = N s. The wave function (5.24) represents a gas rotating around the z-axis with tangential velocity (see eqn (5.12)) vs =

s . mr

(5.25)

This law is completely diﬀerent from the rigid rotational ﬁeld v = Ω × r which is also tangential, but whose modulus increases with r (see Figure 5.1). The circulation of the velocity ﬁeld over a closed contour around the z-axis is given by vs · dl = 2πs . (5.26) m and turns out to be quantized in units of h/m, independent of the radius of the contour. This is the consequence of the fact that the vorticity of the velocity ﬁeld (5.25) is concentrated on the z-axis according to the law curlvs = 2πs

(2) δ (r⊥ )ˆ z, m

(5.27)

ˆ is the unit vector in where r⊥ is a two-dimensional vector in the x, y plane, and z the z-th direction. Results (5.24) and (5.27) show that the irrotationality criterion, associated with the occurrence of Bose–Einstein condensation, is satisﬁed everywhere except on the line of the vortex. Substituting (5.24) into eqn (5.18) we obtain the following equation for |Ψ0 |: d|Ψ0 | 2 s 2 2 1 d r + − |Ψ0 | + g|Ψ0 |3 − μ|Ψ0 | = 0. (5.28) 2m r dr dr 2mr2 5 4 virr 3

vrig

v 2 1 0

0

1

2

3

4

5

r [a.u.]

Figure 5.1 Tangential velocity ﬁeld for irrotational (virr ) and rigid rotational (vrig ) ﬂow. The irrotational velocity ﬁeld diverges like 1/r as r → 0. Here r and v are measured in arbitrary units (a.u.).

50

Nonuniform Bose Gases at Zero Temperature

At large distances from the vortex line the density √ of the gas must approach its unperturbed uniform value n and hence |Ψ0 | → n. This suggests the introduction of the dimensionless function |Ψ0 | =

√

nf (η),

(5.29)

√ where η = r/ξ and ξ = / 2mgn is the healing length. The real function f (η) satisﬁes the equation 1 d df s2 η + 1 − 2 f − f 3 = 0, (5.30) η dη dη η with the constraint f (∞) = 1. For η → 0 the physical solution of (5.30) tends to zero as f ∼ η |s| , so the density n(r) = |Ψ0 (r)|2 of the liquid tends to zero on the axis of the vortex. From the dimensionless nature of eqn (5.30) one sees that the core of the vortex line, i.e. the region near the axis where the density is perturbed in a signiﬁcant way, is of the order of the healing length ξ. In Figure 5.2 the function f (η) is shown for the values s = 1 and s = 2. The energy of the vortex is calculated by evaluating the integral (5.8) with the wave function (5.24) and subtracting from this expression the ground state energy of the uniform gas occupying the volume V = LπR2 of the cylinder. This subtraction, however, should be made at ﬁxed N and should hence take into account the changes of the density of the gas at large distances, due to the presence of the vortical line. We can avoid this problem by carrying out the calculation at ﬁxed chemical potential μ and using the grand canonical energy (5.19). In other words the energy of the vortex line is calculated as Ev = E − Eg , where Eg = V gn2 /2 − μV n. Now we can safely 1 0.8 0.6 f (η) 0.4 0.2 0

0

1

2

3 η

4

5

6

Figure 5.2 Vortical solutions (s = 1, solid line; s = 2, dashed line) of the Gross–Pitaevskii equation as a function of the radial coordinate r/ξ. The density of the gas is given by n(r) = nf 2 , where n is the density of the uniform gas.

Vortex rings

51

introduce the chemical potential μ = gn into Ev , because corrections to μ, due to the presence of the vortical line, are negligible. In terms of the dimensionless function f we have Lπ2 n Ev = m

R/ξ

df dη

2

2 s2 2 1 2 f −1 ηdη . + 2f + η 2

(5.31)

0

Integration of (5.31) with proper accuracy yields the result (Pitaevskii, 1961) 1.46R 2 (5.32) Ev = Lπn ln m ξ for the excitation energy of the s = 1 vortex, holding for R ξ. The main contribution to Ev comes from the kinetic energy which provides the leading term arising from the large r behaviour of the velocity ﬁeld (5.25). The energy Ev is macroscopically large since it increases with the size the sample as L ln R. The relative change Ev /Eg with respect to the ground state energy is, however, vanishingly small in the thermodynamic limit. This is consistent with the fact that the chemical potential of the gas has not changed in the same limit. Result (5.32) has been derived in the laboratory frame. In a frame rotating with angular velocity Ω one should consider the Hamiltonian H = H0 − ΩLz ,

(5.33)

where H0 ad Lz are, respectively, the Hamiltonian and the angular momentum in the laboratory frame. It is then easy to see that in the rotating frame the vortex solution, which carries angular momentum Lz = N , becomes energetically favourable with respect to the ground state solution of H0 if Ω is suﬃciently high. This happens for angular velocities larger than the critical value Ev 1.46R Ωc = = . (5.34) ln N mR2 ξ

5.4

Vortex rings

In addition to the vortex conﬁguration discussed in the preceding section one can also study solutions corresponding to vortex lines of more complicated form. In this section we consider the so-called vortex rings, i.e. closed vortex lines of circular form with radius R0 (see Figure 5.3). These solutions are associated with a localized perturbation of the density proﬁle moving with respect to the ﬂuid at constant velocity. They consequently correspond to stationary solutions of the Gross-Pitaevskii equation in the frame moving with the velocity of the ring. For large rings, such that R0 ξ, the energy of the vortex can be easily calculated starting from the results discussed in the preceding section. In fact, in this case it is possible to introduce a cut-oﬀ distance Rc which separates the region near the vortex line (r⊥ Rc ) from the region far from the line (r⊥ Rc ). Here r⊥ is the distance

52

Nonuniform Bose Gases at Zero Temperature

R0

Figure 5.3 For large vortex rings the phase S exhibits a discontinuity on the surface enclosed by the ring.

from the vortex line and Rc should satisfy the condition ξ Rc R0 . In the ﬁrst region one can consider the vortex as a straight line and its energy can be calculated directly by employing eqn (5.32). In the second region the gas can be treated as an incompressible ﬂuid whose excitation energy arises from the kinetic energy term. The sum of the two contributions does not depend on Rc and one obtains the simple result (Amit and Gross, 1966; Roberts and Grant, 1971) 2 1.59R . (5.35) (R0 ) = 2π 2 R0 n ln m ξ A peculiar feature of the vortex ring is that the corresponding velocity ﬂow gener ates a net momentum p = m drnvs . This can easily be calculated for large rings. In fact, if ξ R0 onecan neglect the density inhomogeneity produced by the vortex line and write p = mn dr∇S. This integral can be transformed into the surface integral mn dsS, where the surface should include a cut characterized by the 2π discontinuity of the phase S. The integral ﬁnally yields the result p = 2π 2 nR02 n,

(5.36)

where n is the unit vector perpendicular to the ring. One should, however, recall that the velocity vs decreases at large distances like 1/r 3 so that the contribution from the remote surface containing the ring cannot be ignored without further considerations. We can always consider a nonstationary conﬁguration corresponding to the creation of the ring at some initial time. Then for large, but ﬁnite times, the velocity vs is equal to zero at inﬁnity and the integral over the remote surface vanishes (see also Pitaevskii, 2014).

Vortex rings

53

In contrast to the straight vortex line, the vortex ring is not at rest, but moves with velocity v=

d/dR0 d = , dp dp/dR0

(5.37)

and explicit diﬀerentiation yields the result ln v= 2mR0

4.32R , ξ

(5.38)

which holds for large rings satisfying the condition R0 ξ. Equation (5.38) shows that the velocity becomes smaller and smaller as the size of the ring increases. Starting from the Gross-Pitaevskii equation it is also possible to obtain solutions for rings with size comparable to the healing length and for which results (5.35)–(5.38) do not apply. Let us consider a ring with its centre on the z-axis and moving in the z-direction. One can look for a solution of the equations of motion in the form Ψ (r, t) = Ψ0 (r, z − vt) e−iμt/ ,

(5.39)

where the velocity v is a constant parameter. Let us introduce the dimensionless cylindrical variables η = r/ξ and ζ = (z − vt) /ξ and write the order parameter as Ψ0 (r, z − vt) =

√

nf (η, ζ).

(5.40)

Substituting eqn (5.40) into (5.2), we ﬁnd the following equation for the wave function f : 2iU

1 ∂ ∂f = ∂ζ η ∂η

∂f ∂2f 2 η + 2 + f (1 − |f | ), ∂η ∂ζ

(5.41)

where the dimensionless velocity U is deﬁned by U=

v mvξ = √ , c 2

(5.42)

where c is the usual velocity of sound and we have set μ = gn. Equation (5.41) should be solved subject to the boundary conditions f → 1 when η, ζ → ∞. This problem was solved by Jones and Roberts (1982). The important quantities to calculate are the energy and the momentum of the ring. The excitation energy can be calculated by subtracting the energy of a uniform gas from (5.8). Similar to the calculation of the vortex energy it is convenient to use the grand canonical energy E . In terms of the dimensionless variables one can write = E − Eg =

2 ξn , m

(5.43)

54

Nonuniform Bose Gases at Zero Temperature

with 1 = 2

2 2 2 ∂f ∂f 1 2 + + 1 − |f | 2πηdηdζ . ∂η ∂ζ 2

(5.44)

For the momentum of the vortex ring one instead ﬁnds the result p = nξ 2 p, with i p = 2

∂f ∗ ∂f ∗ (f − 1) − (f − 1) 2πηdηdζ. ∂ζ ∂ζ

(5.45)

(5.46)

In deriving result we have subtracted from the total momentum m drn∇S the (5.46) quantity (inξ) (∂f ∗ /∂ζ − ∂f /∂ζ)πηdηdζ, which can be transformed into an integral on the remote surface and, according to the arguments discussed after eqn (5.36), can be safely set equal to zero. This ensures the convergency of the integral (5.46). A remarkable feature of the above formalism is that the velocity v of the ring, entering the ansatz (5.39) for the solution of the Gross-Pitaevskii equation, exactly satisﬁes the relationship v = d/dp or, in dimensionless units, U = d /d p. This can be formally proven using eqn (5.41) and results (5.44) and (5.46). The calculation of and p reveals interesting features. At small velocities U , corresponding to large rings, the energy and the momentum approach the results (5.35) and (5.36) and the phase of f acquires the value 2π around the vortical line. The radius of the ring decreases as U increases and for U = U1 = 0.62, corresponding to v = 0.88c, it becomes equal to zero. For U > U1 the phase of the order parameter becomes single valued. Furthermore, both and p have a minimum at U = U2 = 0.66. This means that in the − p plane there are two branches of solutions, with a bifurcation √ at U = U2 (see Figure 5.4). The upper branch is unstable. Since the value U = 1/ 2 = 0.71 corresponds to v = c, the velocity U2 of the excitation with the minimal energy is of the order, but smaller than, the velocity of sound. The velocity of the ring approaches the sound velocity for the excitations of the upper branch in the asymptotic limit p, → ∞. It is also worth noticing that the 1/2 minimum value of the energy scales (see eqn (5.43)) like 2 ξn/m ∼ μ/ na3 and is consequently much larger than the typical energies of the elementary excitations, ﬁxed by the chemical potential. Another interesting problem is the one of vortex pairs, corresponding to two parallel vortices of opposite circulation and separated by a distance d. The problem can be easily solved if d ξ. In this case the energy and momentum are calculated using the same procedure yielding eqns (5.35) and (5.36). Within logarithmic accuracy one ﬁnds the results n2 d = 2π ln (5.47) m ξ for the energy per unit length, and p = 2πnd

(5.48)

Solitons

55

68

60 ε˜ 52

44 65

• U1 = 0.62

• U2 = 0.66 p˜ 2 p˜ 1

70

75

80

85

90

95

100

p˜

Figure 5.4 Energy–momentum diagram for a vortex ring in reduced units (see text). The lower branch is stable, and for p˜ p˜1 the circulation of the velocity ﬁeld around the vortical line is diﬀerent from zero. The upper branch is unstable. Its velocity approaches the sound √ velocity (U = 1/ 2) for p˜ 1.

for the momentum per unit length. Similar to the ring, a vortex pair is not at rest, but moves with velocity v = d/dp = /md. Vortex pairs can also be investigated in the more microscopic regime where d is of the order of the healing length or smaller. In this case it is convenient to rewrite eqn (5.41) in terms of the dimensionless Cartesian coordinates x/ξ and y/ξ (vortices are aligned along the z-th axis), and to express the energy and momentum per unit of length in the form = (2 /m)n and p = nξ p, respectively, where and p are dimensionless quantities. The solutions can again be discussed as a function of the reduced velocity U = mvξ/ (see eqn (5.42)). The properties of the new solutions are, however, diﬀerent with respect to those found in the rings. There is again a critical value of the velocity taking place at U = U1 = 0.5. If U < U1 there are two points where the order parameter vanishes, corresponding to a vortex pair. However, the separation d between the two vortices tends to zero when U → U1 . For U > U1 the solution no longer corresponds to a vortex pair, but rather to a localized density perturbation without any singularity. Such a solution also exists in the limit p → 0 √ where U → 1/ 2 and v → c (Jones and Roberts, 1982). The dispersion law of the vortex pair excitation is shown in Figure 5.5.

5.5

Solitons

In this section we will consider special solutions of the time-dependent Gross-Pitaevskii eqns (5.2) called solitons. In the case of repulsive forces these solutions correspond to a localized modulation of the density proﬁle moving in the medium at constant velocity, in such a way that the intrinsic shape of the system is preserved in time. The proﬁle

56

Nonuniform Bose Gases at Zero Temperature

12 phonon line

ε˜

• U1 = 0.5

6

p˜ 1 0

0

10 p˜

5

15

20

Figure 5.5 Energy–momentum diagram for a vortex–antivortex pair in reduced units. For small momenta the slope approaches the sound velocity.

in the perturbed region is characterized by a suppression of the density with respect to the bulk value (grey soliton). The existence of grey solitons is directly related to the nonlinearity of the GP equations, whose eﬀect is compensated by the quantum pressure term arising from the kinetic energy. The typical length characterizing the extension of the density modulation is then ﬁxed by the healing length. In the present section we will consider one-dimensional solutions, where the order parameter Ψ0 depends only on the coordinate z, through the combination z − vt. Introducing the √ dimensionless variables as in eqn (5.40), one can write Ψ (z, t) = Ψ0 (z − vt) e−iμt/ ≡ nf (ζ)e−iμt/ obtaining, by analogy with (5.41), the equation 2iU

d2 f df 2 = + f (1 − |f | ), dζ dζ 2

(5.49)

(z − vt) ξ

(5.50)

where ζ=

and now the wave function does not depend on the ‘radial’ variable η. Our goal is to construct a ‘localized’ solution satisfying the boundary conditions |f | → 1,

df →0 dζ

(5.51)

as ζ → ±∞. By multiplying eqn (5.49) by f ∗ and subtracting the complex-conjugated equation one ﬁnds, after a simple integration, 2

U (1 − |f | ) + f1

df2 df1 − f2 = 0, dζ dζ

(5.52)

Solitons

57

which is consistent with the boundary conditions (5.51), where f1 and f2 are, respectively, the real and imaginary part of the complex function f = f1 + if2 . Equation (5.52) is actually the continuity eqn (5.9) expressed in the new variables. A second equation for the function f can be derived by taking the imaginary part of (5.49). One ﬁnds: 2U

df1 d2 f2 2 = + f2 (1 − |f | ). dζ dζ 2

(5.53)

Exclusion of df1 /dζ from the last two equations gives: f2

d2 f2 df2 2 2 + f2 − 2U 2 (1 − |f | ) = 0. − 2U f1 2 dζ dζ

(5.54)

√ This equation has an obvious solution f2 = 2U = v/c, satisfying the second boundary condition (5.51). Substitution into (5.52) yields the equation √ df1 = 2 dζ

v2 2 1 − 2 − f1 c

(5.55)

for the real part f1 . Integration of (5.55) is straightforward and yields the nontrivial result (Tsuzuki, 1971) Ψ0 (z − vt) =

√

v n i + c

v2 z − vt v2 1 − 2 tanh √ 1− 2 c c 2ξ

(5.56)

for the time and space evolution of the order parameter, where we have reintroduced the initial physical variables. The density proﬁle takes the form n(z − vt) = |Ψ0 |2 = n + δn (z − vt), with

v2 δn(z − vt) = −n 1 − 2 c

cosh

−2

z − vt √ 2ξ

v2 1− 2 . c

(5.57)

Thus the density has a minimum in the centre of the soliton corresponding to n(0) = nv 2 /c2 (see Figure 5.6). This value is equal to zero for a soliton propagating with zero velocity (dark soliton). It is also worth noticing that the width of the soliton is ﬁxed by the healing length ξ, but is ampliﬁed by the factor 1/ 1 − v 2 /c2 , which becomes increasingly large as v → c. Notice also that the phase of the wave function undergoes a ﬁnite change v ΔS ≡ S(+∞) − S (−∞) = −2 arccos (5.58) c as z varies from −∞ to +∞. For a dark soliton the function Ψ0 is real and odd and the phase change is given by ΔS = −π.

58

Nonuniform Bose Gases at Zero Temperature 1.2

n(z/ξ)

0.8

0.4 v2 = 0.2 c2

0 −8

−4

0 z/ξ

4

8

Figure 5.6 Density proﬁle of a ‘grey’ soliton. The width of the soliton is proportional to the healing length ξ and becomes increasingly large as the velocity of the soliton approaches the sound velocity.

The energy of the soliton per unit surface can be evaluated by taking the diﬀerence between the grand canonical energies in the presence (E ) and in the absence (Eg ) of the soliton. The resulting expression 2 ∞ 2 2 dΨ0 g 2 |Ψ0 | − n = dz (5.59) + 2m dz 2 −∞

can be easily calculated by changing the integration variable from z to f1 and evaluating df1 /dz with the help of (5.55). The ﬁnal result is 3/2 3/2 v2 4 mv 2 4 μ3/2 1 − = cn 1 − 2 = √ , (5.60) 3 c 3 mg μ where, in the second identity, we have expressed the energy of the soliton per unit surface in terms of the velocity and of the chemical potential. The solitonic solution derived above exhibits some intriguing features which are worth discussing. First one notes that for small values of v the soliton, according to eqn (5.60), behaves like a particle with negative mass ms = − 4n/c in accordance with the fact that the density perturbation (5.57) actually corresponds to a hole rather than to a particle. Another nontrivial feature of solitons concerns their momentum. In fact, while according to eqn (5.57) the velocity v determines in an explicit way the time evolution of the density proﬁle, the identiﬁcation of the momentum of the soliton requires a more careful discussion. One can easily calculate the momentum p = m dzjz associated with the current jz = n(z)∂z S carried by the wave function (5.56). The result is v v2 p = −2n 1− 2. (5.61) c c

Solitons

59

We will call this quantity the ‘local momentum’, as the main contribution to the current is produced in a region of space of the order of the width of the soliton. However, p is not the full momentum of the soliton because of the occurrence of a counterﬂow taking place at large distances, which should compensate the asymptotic phase change (5.58). The counterﬂow carries momentum Δp = −n ∂z Sdz = −nΔS, but does not contribute to the energy, due to the large extension occupied by the counterﬂow. This eﬀect is well understood if one considers a soliton built in a torus with a very large radius. Since the wave function should be single valued and at large distances from the soliton the phase diﬀerence is given by eqn (5.58), then the extra contribution Δp to the momentum should arise from the remaining region of the torus where the density is uniform. In conclusion, the total momentum of the soliton is pc = p + Δp, that is

v v v2 − pc = p − nΔS = 2n arccos (5.62) 1− 2 . c c c It is not diﬃcult to check that the momentum (5.62) satisﬁes the canonical relationship v = (∂/∂pc ) = (∂/∂v)(∂v/∂pc ). Thus the momentum pc is the canonical momentum of the soliton. Notice also that pc is just the momentum, which should be transferred to the ﬂuid to create the soliton and is the quantity which should be conserved, for example, in decay processes. For more detailed discussions see Jones and Roberts (1982), Shevchenko (1988), and Scott et al. (2011). For small velocities the local momentum tends to zero. The canonical momentum instead approaches the ﬁnite value πn, due to contribution of the counterﬂow. As v → c, eqn (5.62) gives pc ≈

4n 3

3/2 v2 1− 2 = , c c

(5.63)

expressing the phonon-like nature of the perturbation in this limit. The solution discussed above is actually unstable with respect to ﬂuctuations of the density proﬁle along the transverse x and y directions (Kuznetsov and Turitsyn, 1988). Experimentally the instability can be suppressed by working with suitable geometries of conﬁnement, for example using cigar-shaped traps (Burger et al., 1999, Denschlag et al., 2000). It is ﬁnally worth noting that the velocity of the soliton increases when its energy decreases. This implies that dissipative eﬀects, due, for example, to collisions with thermal excitations, will result in an acceleration of the soliton which will eventually disappear when v → c. If the interaction is attractive (a < 0) the GP equation admits another kind of solitonic solution which corresponds to a localized wave packet in the z-th direction (bright soliton). It is actually easy to check that the time-independent GP equation (5.18) is solved by the wave function Ψ0 (z) = Ψ0 (0)

1 √ , cosh[z/ 2ξ]

(5.64)

60

Nonuniform Bose Gases at Zero Temperature

where n0 = |Ψ0 (0)|2 is the central density and we have deﬁned ξ = / The chemical potential corresponding to this solution is given by 1 μ = − |g|n0 2

2m | g | n0 .

(5.65)

and is negative. This wave packet can move freely in space along the z-th direction like an ordinary particle. Bright solitons are not, however, stable conﬁgurations. They can be produced in traps with tight radial conﬁnement where the mechanism of destabilization is reduced (Khaykovich et al., 2002; Strecker et al., 2002).

5.6

Small-amplitude oscillations

An important class of time-dependent solutions of the GP equation is small-amplitude oscillations, where the changes in space and time of the order parameter with respect to the stationary conﬁguration are small. In many cases these solutions emphasize the collective behaviour exhibited by interacting Bose gases. In this section we present the general formalism of these oscillations, based on the classical GP theory. The smallamplitude oscillations can also be interpreted in terms of the elementary excitations of the system and they admit a natural quantum description which will be discussed later in this section. Many examples will be illustrated in the following chapters. In addition to the small-amplitude oscillations one can also explore large-amplitude solutions, including the most important problem of the expansion of the gas after releasing the trap. This problem will be addressed directly in Section 12.7. The small oscillations of the system around equilibrium can be investigated by writing the order parameter in the form Ψ(r, t) = Ψ (r, t)e−iμt/ = [Ψ0 (r) + ϑ(r, t)]e−iμt/ , where ϑ is a small quantity for which we look for solutions of the form [ui (r)e−iωi t + vi∗ (r)e+iωi t ], ϑ(r, t) =

(5.66)

(5.67)

i

where ωi is the frequency of the oscillation. Note that, using eqn (5.7), the GP equation for Ψ (r, t) can be written as i

δE ∂Ψ (r, t) = , ∗ ∂t δΨ0 (r, t)

(5.68)

where E is the grand canonical energy (5.19). The functions ui (r) and vi (r) are determined by solving the Gross-Pitaevskii equation in the linear limit. By collecting all the terms evolving in time like e−iωi t/ and eiωi t/ one obtains the following pair of diﬀerential equations (Bogoliubov equations). ˆ 0 − μ + 2gn(r))ui (r) + g(Ψ0 (r))2 vi (r), ωi ui (r) = (H ˆ 0 − μ + 2gn(r))vi (r) + g(Ψ∗0 (r))2 ui (r), −ωi vi (r) = (H

(5.69)

Small-amplitude oscillations 2

61

2

ˆ 0 = − ∇ + Vext (r) and the index i labels the i-th solution. The formalism where H 2m of eqns (5.69) was developed by Pitaevskii (1961) to describe the oscillations of a vortex line. Equations (5.69) provide the eigenfrequencies and the amplitudes u and v of the normal modes of the system. In general they must be solved numerically. An analytically soluble example is provided by the collective oscillations around the ground state of a uniform gas (Vext =√0), where μ = gn and Ψ0 is independent of r and can be chosen to be real (Ψ0 = n). In this case one ﬁnds the solutions u(r) = ueik·r and v(r) = veik·r , and eqn (5.69) reduces to ωu =

2 k 2 u + gn(u + v), 2m

−ωv =

2 k 2 v + gn(u + v). 2m

Equations (5.70) admit the analytic solution 2 2 2 k 2 k 2 2 gn (ω) = + 2m m

(5.70)

(5.71)

for the frequency as a function of the wave vector k. Equation (5.71) coincides with the Bogoliubov dispersion law (4.31) after setting p = k and = ω. The solutions of (5.69) exhibit important properties that are worth discussing. First, by taking suitable combinations of these equations one easily ﬁnds the result (ωi − ωi∗ ) dr |ui |2 − |vi |2 = 0, (5.72) which shows that, unless dr|ui |2 = dr|ui |2 , the Bogoliubov equations (5.69) only admit solutions with a real frequency. The occurrence of a complex frequency is associated with a dynamic instability of the system. In the following we will only consider dynamically stable conﬁgurations. A second important property is that two solutions with frequencies ωi = ωj satisfy the orthogonality relation (5.73) (u∗i uj − vi∗ vj )dr = 0. Furthermore, for each solution ui and vi with frequency ωi there exists another solution vi∗ and u∗i with frequency −ωi . The two solutions represent the same physical oscillation as one can easily see by looking at eqn (5.67). It is also worth noticing that ωi = 0 is always a solution of (5.69) with u = αΨ0 and v = −αΨ∗0 . In this case the order parameter (5.66) takes the form Ψ0 (r, t) = Ψ0 (r)(1 + (α − α∗ )) exp[−iμt/], corresponding to a gauge transformation in which the phase of the order parameter is modiﬁed by the quantity (α − α∗ )/i. This transformation does not result in any physical excitation of the system. A useful quantity is the energy change associated with the small oscillations (5.66) around equilibrium. Since the deﬁnition of ϑ (5.66) contains the chemical potential μ

62

Nonuniform Bose Gases at Zero Temperature

explicitly, it is convenient to start from the calculation of the grand canonical energy E deﬁned in (5.19). The potential E has the property that its value, for a given choice of μ, is stationary when Ψ = Ψ0 . This implies that in E the terms which are linear in ϑ, ϑ∗ vanish and that consequently, up to terms quadratic in ϑ and ϑ∗ , we can write E = E0 + E (2) ,

(5.74)

where the equilibrium value E0 is simply obtained by inserting the stationary solution Ψ0 (r) into eqns (5.8) and (5.19). The term E (2) , being quadratic in ϑ, ϑ∗ , satisﬁes the Euler identity

δE (2) δE (2) ∗ ϑ (r) + ϑ (r) ∗ dr = 2E (2). (5.75) δϑ(r) δϑ (r) On the other hand, from the variational eqn (5.68) it follows that the function ϑ satisﬁes the equation i

∂ϑ(r) δE (2) = ∗ ∂t δϑ (r)

which, inserted into eqn (5.75), yields the result

i ∂ϑ(r) ∂ϑ∗ (r) (2) ∗ E = ϑ (r) − ϑ (r) dr 2 ∂t ∂t

(5.76)

(5.77)

Substituting expression (5.67) for ϑ and using the orthogonality relations (5.73), one ﬁnally ﬁnds the expression E (2) = dr(|ui |2 − |vi |2 )ωi (5.78) i

for the energy change. One can now use the theorem of ‘small increments’ (Landau and Lifshitz, 1980, Section 24) according to which the perturbative corrections to E and E coincide if calculated at ﬁxed N and μ respectively. This implies that the energy relative to the time-dependent solution is given by E = E0 + E (2) ,

(5.79)

with the same value E (2) entering the grand canonical energy. Equation (5.78) explicitly shows that the quantity dr(|ui |2 − |vi |2 )ωi must be positive for each mode in order to ensure the stability of the system. The occurrence of solutions for which the above quantity is negative is a direct signature of an energetic instability and reveals that the stationary solution Ψ0 does not correspond to a minimum of the energy functional (5.8). The energetic instability should not be confused with the dynamic instability associated with the appearance of an imaginary component in the value of ωi . In contrast to the dynamic instability, the energetic instability can destabilize the system in the presence of dissipative terms which drive it

Small-amplitude oscillations

63

towards conﬁgurations with lower energy. Important examples of such instabilities are found in the study of quantized vortices and will be discussed in the Part II of this volume (see Chapter 14). Finally, it is useful to express the integral dr(|ui |2 − |vi |2 ) entering the energy (5.78) in terms of the variations δni and δSi of the density and of the phase, respectively, of the order parameter (5.11) associated with the corresponding solution. + The comparison with eqns (5.66) and (5.67) shows that ui = δn+ Ψ0 i /(2n0 ) + iδSi + + and vi = δni /(2n0 ) − iδSi+ Ψ0 , where δn+ and δS are deﬁned by i i −iωi t +iωi t δni (r, t) = δn+ + δn− , i (r)e i (r)e

(5.80)

δSi (r, t) = δSi+ (r)e−iωi t + δSi− (r)e+iωi t .

(5.81)

This yields the identity − dr(|ui |2 − |vi |2 ) = −i dr δn+ i δSi − c.c. .

(5.82)

Results (5.78) and (5.82) can be used to explore the conditions of stability employing the formalism of hydrodynamics where the normal modes are naturally described in terms of small oscillations of the density and of the phase S (see Section 5.2), rather than in terms of the amplitudes u and v. The solutions of the linearized Gross-Pitaevskii equations provide the eigenfrequencies corresponding to the small oscillations of the system. The interpretation of these solutions in terms of the eigenstates of the many-body Hamiltonian requires a procedure of quantization (Fetter, 1972). In the formalism of second quantization the Hamiltonian can be obtained from eqn (5.8) by replacing the classical ﬁeld Ψ with the ˆ and takes the form corresponding ﬁeld operator Ψ, ˆ = H

2 2 g ∇ † ˆ ˆ ˆ † (r)Ψ(r ˆ )Ψ(r), ˆ ˆ † (r )Ψ drΨ (r) − + Vext Ψ(r) + drdr Ψ 2m 2

(5.83)

where we have properly taken into account the order of the ﬁeld operators. It is useful to work in the Heisenberg representation and write the Bose-ﬁeld operator in the form ˆ (r, t) = Ψ0 (r) + ϑˆ (r, t) e−iμt/ , (5.84) Ψ ˆ in analogy with the classical ﬁeld (5.67), is where the operator ϑ, ˆ t) = ϑ(r,

[ui (r)ˆbi e−iωi t + vi∗ (r)ˆb†i eiωi t ].

(5.85)

i

Here ui , vi , and ωi are the solutions of the Bogoliubov equations (5.69) and ˆbi and ˆb†i are, respectively, the annihilation and creation operators of the i-th elementary excitation, satisfying the usual Bose commutation rule [bi , b†j ] = δij and zero otherwise.

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Nonuniform Bose Gases at Zero Temperature

Then, substituting (5.85) into (5.83) and using the orthogonality property (5.73) holding for the solutions of the linearized time-dependent Gross-Pitaevskii eqns (5.69), we obtain the expression (2) H = (5.86) drωi (|ui |2 − |vi |2 )ˆb†i ˆbi , i

which replaces the classical term (5.78) and where we have omitted a constant term arising from the commutation between the operators ˆbi and ˆb†i . The proper calculation of this constant term, which contributes to the ground state energy, requires the renormalization of the scattering length, as discussed in the uniform case. The operator (5.86) takes the form H (2) = ωiˆb†i ˆbi (5.87) i

of the Hamiltonian of a gas of independent quasi-particles if the solutions of (5.69) are normalized to unity, i.e. if they satisfy the ortho-normalization conditions (5.88) [u∗i (r)uj (r)–vi∗ (r)vj (r)] dr = δij . With such a choice for the normalization the frequencies ωi of the elementary excitations will be positive if the i-th solution is energetically stable, while they will be negative in the opposite case. The condition of normalization concludes the procedure of quantization, which generalizes to the case of nonuniform gases the Bogoliubov results presented in the previous chapter. Finally, it is worth pointing out that the ground state of the Hamiltonian (5.87) diﬀers from the Hartree–Fock many-body wave function (5.5). In fact, it corresponds to the vacuum of quasi-particles (ˆbi | 0 > = 0) and is characterized by the occurrence of quantum correlations, which give rise to the quantum depletion of the condensate and to important changes in the correlation functions, as has already been discussed in the case of the uniform interacting gas in Chapter 3.

6 Superﬂuidity Superﬂuidity is strongly related to the phenomenon of Bose–Einstein condensation. Superﬂuids can ﬂow through narrow capillaries or slits without dissipating energy, their shear viscosity being equal to zero. The superﬂuidity of liquid 4 He, below the so-called λ-point, was discovered by Kapitza (1938) and, independently, by Allen and Misener (1938). The phenomenon was soon explained by Landau (1941) who showed that, if the spectrum of elementary excitations satisﬁes suitable criteria, the motion of the ﬂuid cannot give rise to dissipation. In the present chapter we develop Landau’s argument and discuss the crucial role played by irrotationality in characterizing the superﬂuid motion. Irrotationality is directly related to Bose–Einstein condensation, being naturally associated with the phase of the order parameter which ﬁxes the shape of the velocity potential. In this chapter we also discuss the main features of the hydrodynamic theory of superﬂuids which provides a general description of the dynamical behaviour of such systems at a macroscopic level. The hydrodynamic theory permits, in particular, the calculation of the ﬂuctuations of the phase of the order parameter, providing a further link between superﬂuidity and Bose–Einstein condensation. In the last part of this chapter we will focus on the rotational properties, with special emphasis on the behaviour of quantized vortices. Some of the important features exhibited by superﬂuids (irrotationality, applicability of hydrodynamic theory, and occurrence of quantized vortices) have already been discussed in the previous chapter, which was devoted to dilute Bose gases. In this chapter we show that these concepts have a broader range of applicability, including the most famous cases of superﬂuid 4 He and of superﬂuid Fermi gases. This also permits better clariﬁcation of the conceptual diﬀerence between superﬂuidity and Bose–Einstein condensation, a distinction which does not always emerge clearly in three-dimensional dilute gases.

6.1

Landau’s criterion of superﬂuidity

A major role in Landau’s theory of superﬂuids is played by the transformation laws of energy and momentum under Galilean transformations. Let E and P be, respectively, the energy and the momentum of the ﬂuid in a reference system K. The energy and the momentum in the system K , moving with velocity V with respect to K, are given by 1 E = E − P · V + M V 2 , P = P − M V, 2

(6.1)

where M is the total mass of the ﬂuid.

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

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Superﬂuidity

Let us ﬁrst consider a uniform ﬂuid at zero temperature ﬂowing along a capillary at constant velocity v. If the ﬂuid is viscous the motion will produce dissipation of energy with consequent heating and decrease of the kinetic energy. In the following we will consider only dissipative processes taking place through the creation of elementary excitations. Let us describe the process in the reference frame moving with the ﬂuid. If a single excitation with momentum p appears in the ﬂuid then the total energy is E0 + (p), where E0 and (p) are, respectively, the energy of the ground state and of the excitation, while the momentum carried by the ﬂuid is given by p. Let us now go to the reference system where the capillary is at rest. In this frame, which moves with respect to the ﬂuid with velocity −v, the energy E and momentum P are given, according to (6.1), by 1 E = E0 + (p) + p · v + M v 2 , P = p + M v . 2

(6.2)

Equation (6.2) shows that the quantities (p) + p · v and p are, respectively, the change in energy and in momentum due to the appearance of the excitation. Thus we can conclude that (p) + p · v is the energy of an elementary excitation in the frame where the capillary is at rest. The crucial point now is that the process of spontaneous creation of excitations can take place only if it is energetically ‘proﬁtable’, i.e. if the excitation energy is negative: (p) + p · v < 0.

(6.3)

This is possible if v > (p)/p and, of course, we assume that the sample can transfer the momentum p to the capillary. In this case the ﬂow of the ﬂuid is unstable and its kinetic energy will be transformed into heat. If instead the velocity is smaller than the value vc = min p

(p) , p

(6.4)

where the minimum is calculated over all the values of p, then the condition (6.3) is never satisﬁed and no excitation will spontaneously grow in the ﬂuid. Landau’s criterion for superﬂuidity can then be written in the form v < vc ,

(6.5)

and ensures that if the relative velocity between the ﬂuid and the capillary is smaller than the critical value (6.4) then there will be a persistent ﬂow without friction. The realized conﬁguration corresponds to a state of metastable equilibrium. It is in fact stable with respect to the creation of elementary excitations, but diﬀers from full thermodynamic equilibrium where the whole system is at rest. Examples of metastable currents and of possible decay mechanisms will be discussed in Section 14.9 in the context of toroidal conﬁgurations. By looking at the Bogoliubov excitation spectrum (4.31), one easily concludes that the weakly interacting Bose gas fulﬁls the Landau criterion for superﬂuidity and that the critical velocity is given by the velocity of sound. Strongly interacting superﬂuids

Landau’s criterion of superﬂuidity

67

like 4 He also meet Landau’s criterion, although in this case the critical velocity is smaller than the sound velocity due to the more complex structure of the excitation spectrum. According to the Landau criterion given in (6.4) and (6.5), the ideal Bose gas is instead not superﬂuid. In fact, in this case (p) = p2 /2m and the value of vc is equal to zero. Landau’s criterion (6.4) for the critical velocity can be also derived using a diﬀerent approach, based on the inclusion of a heavy impurity moving with velocity v with respect to the ﬂuid at rest and generating a weak perturbation on the ﬂuid of the form U (r − vt) = dq exp(iq · (r − vt))Uq , where Uq is the Fourier transform of the perturbation. Using the formalism of response function theory (see Chapter 7) it is then easy to prove that the Fermi golden rule gives rise to ﬁnite transitions in the ﬂuid, generating dissipation, only if v ≥ (p)/p, where (p) is the excitation spectrum of the ﬂuid and p = q. The approach of the moving impurity will be employed in Section 24.5 to calculate the friction force in a one-dimensional Bose gas. Let us now consider a uniform ﬂuid at ﬁnite, although small, temperature, and let us assume that the thermodynamic properties of the system are equivalent to those of a gas of non-interacting excitations (quasi-particles) in thermal equilibrium. These quasi-particles can transport part of the mass of the system, but, in virtue of the arguments discussed above, no new excitations can be created because of the motion of the superﬂuid with respect to the capillary. The additional mass ﬂow associated with the thermally excited quasi-particles is not superﬂuid. These excitations can collide with the walls of the capillary and exchange momentum and energy. Because of these collisions new excitations can be created in the system, and the corresponding motion will exhibit dissipation like in ordinary ﬂuids. Thus we have the following scenario: at non-zero temperature part of the ﬂuid behaves as a normal viscous liquid, while the remaining part behaves as a superﬂuid without viscosity. Collisions establish thermodynamic equilibrium in the gas of excitations. At equilibrium the velocity vn of this gas coincides with the velocity of the frame where the capillary is at rest. The relative velocity of the superﬂuid and the capillary is given by vs − vn , so that the energy of elementary excitations in the capillary frame is given by ε(p) + p · (vs − vn ), where ε(p) and p are the energy and the momentum of the excitation in the coordinate system where the superﬂuid is at rest. Correspondingly, the equilibrium distribution function Np of elementary excitations is −1

ε(p) + p · (vs − vn ) − 1 = exp . Np kB T

(6.6)

This equation again reveals the consistency of Landau’s criterion (6.5). In fact, only if the relative velocity |vs − vn | is smaller than the critical velocity vc will the distribution function (6.6) be positive for all values of p. Notice also that the existence of thermodynamic equilibrium characterized by the function (6.6) implies that there is no friction between the normal and superﬂuid components of the liquid. The existence of friction would in fact violate even the meaning of (6.6). According to the picture described above, the mass density of the superﬂuid liquid can be written as the sum ρ = ρs + ρn of a normal and of a superﬂuid component,

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Superﬂuidity

moving with velocities vs and vn respectively (following the standard literature, in this Chapter we will make use of the mass density ρ = nm rather than of the number density n employed in the previous chapters). The mass current of the liquid, i.e. the momentum per unit volume, takes the form mj = ρs vs + ρn vn .

(6.7)

Equation (6.7) permits to derive an explicit form for the normal density of the ﬂuid in terms of the elementary excitations present in the system. Let us go to the frame where the superﬂuid is at rest, i.e. vs = 0. Then mj = ρn vn . On the other hand the total momentum carried by the ﬂuid in this frame can be written as P = p Np p, where the sum is taken on all the elementary excitations. If we rewrite this equation per unit volume we derive the expression dp mj = pNp . (6.8) (2π)3 Comparison of equation (6.7) with (6.8) yields the following equation for the normal density: dp ρn vn = pNp , (6.9) (2π)3 with Np given by eqn (6.6) with vs = 0. Let us now assume that velocity vn is small and expand Np in powers of vn . The zero-order term vanishes while the linear one, after some straightforward algebra, gives the result ρn = −

1 3

dNp (ε) 2 dp p , dε (2π)3

(6.10)

where we have used the fact that the distribution function of elementary excitations is an isotropic function of p. Equation (6.10) is the central result of Landau’s theory of superﬂuidity and permits the calculation of the normal component in terms of the distribution function Np of elementary excitations. We recall, however, that this equation is meaningful only if the elementary excitations are well deﬁned and do not interact. This condition is usually satisﬁed in uniform systems at low enough temperatures. It is, however, violated at higher temperatures and in particular near the critical point where thermal excitations are numerous and interact each other. Even at low temperatures, however, Landau’s formula (6.10) is not applicable in all situations. For example, in the presence of disorder, the concept of elementary excitation is not well deﬁned and the normal component of the ﬂuid should be calculated using diﬀerent procedures. As a simple application of eqn (6.10) we calculate the normal density of the weakly interacting Bose gas discussed in Chapter 3. In the integration (6.10) only energies of the order of kB T are important and, for low temperatures such that kB T μ, only the phonon part of the spectrum contributes to the integral. Putting ε(p) = cp in eqn (6.6) and (6.10) and integrating by parts we obtain the result dNp 2 dp 1 2π 2 (kB T )4 ρn = − p = , (6.11) 3 3u dp (2π) 453 c5

Bose–Einstein condensation and superﬂuidity

69

which shows that the temperature dependence of ρn diﬀers from the one exhibited by the thermal depletion of the condensate (see eqn 4.53), which is of order T 2 at low temperatures. In the opposite limit, kB T μ, the integral (6.10) is dominated by the single-particle part of the spectrum (p) = p2 /2m. In this regime the particle and quasi-particle occupation numbers coincide and one ﬁnds the result dp ρn = m np = mnT , (6.12) (2π)3 showing that, in this case, the normal part coincides with the thermal depletion of the condensate. We stress again, however, that the present calculation is not valid near the critical temperature since it neglects interactions between excitations. It is worth noticing that expression (6.10), applied to the ideal gas where (p) = p2 /2m, would yield result (6.12) for ρn for all values of T , indicating that the system is superﬂuid below Tc . This result seems to contradict the fact that the ideal Bose gas does not meet the Landau criterion for the critical velocity. The contradiction is only an apparent one. In fact, result (6.10) for ρn has been obtained by carrying out a linear expansion of the momentum distribution (6.6) for small values of vs − vn . While for a superﬂuid, where vc = 0, we are always allowed to carry out the expansion and the integral converges uniformly to its linear limit, in the ideal gas not only is the expansion meaningless, but the same deﬁnition of Np given in (6.6) violates the positiveness condition.

6.2

Bose–Einstein condensation and superﬂuidity

Let us now discuss the relation between Bose–Einstein condensation and superﬂuidity. To understand this important connection it is useful to consider the properties of the condensate wave function Ψ0 under Galilean transformations. It is worth noticing that, even if the system is uniform and the condensate density |Ψ0 |2 is constant, the function Ψ0 itself is not Galilean invariant since it acquires a phase factor. This factor is easily ˆ t) calculated by recalling that, in the Heisenberg representation, the ﬁeld operator Ψ(r, obeys the equation (see eqn (5.1) with Vext = 0)

2 2 ∂ ˆ ∇ † ˆ ˆ ˆ + Ψ (r , t)V (r − r)Ψ(r , t)dr Ψ(r, t). i Ψ(r, t) = − ∂t 2m ˆ t) satisﬁes (6.13) then It is immediate to check that if Ψ(r,

1 i 2 ˆ ˆ mv · r − mv t , Ψ (r, t) = Ψ(r − vt, t) exp 2

(6.13)

(6.14)

where v, a constant vector, is a solution. This equation gives the Galilean transformation of the ﬁeld operator that we are looking for. The order parameter, which corresponds to the condensate component of the operator (6.14) or, as discussed in ˆ obeys the same transformation law. In the Chapter 2, to its expectation value Ψ, coordinate system where the sample is in equilibrium, the condensate wave function √ of a uniform ﬂuid is given by Ψ0 = n0 e−iμt/ , where n0 is a constant independent

70

Superﬂuidity

of r. In the frame where the ﬂuid moves with velocity v, the order parameter instead √ takes the form Ψ0 = n0 eiS , where

1 1 2 mv · r − mv + μ t (6.15) S(r, t) = 2 √ is the new phase, while the modulus n0 has not changed. Equation (6.15) shows that the velocity is proportional to the gradient of the phase vs =

∇S m

(6.16)

and can be identiﬁed as the superﬂuid velocity. Although derived for a constant velocity, eqn (6.16) is also valid for vs varying slowing in space and time. This equation establishes the irrotationality of the superﬂuid motion, the phase of the order parameter playing the role of a velocity potential. Notice that in deriving eqn (6.16) we have never assumed that the system is a dilute gas, nor that we work at zero temperature. Result (6.16) is a genuine consequence of Bose–Einstein condensation, i.e. of the existence of the classical ﬁeld Ψ0 , associated with the macroscopic component of the ﬁeld operator. The identiﬁcation of the superﬂuid velocity with the gradient of the phase of the order parameter represents a key relationship between Bose–Einstein condensation and superﬂuidity. It is worth noticing that this relationship does not involve the modulus of the order parameter which, in contrast to the phase S, plays a more indirect role in the theory of superﬂuidity and does not directly aﬀect the thermodynamic properties of the system. In this respect we recall that it would be wrong to identify the condensate density mn0 = m|Ψ0 |2 with the superﬂuid density ρs . The distinction between these quantities is already clear at T = 0, where, according to the above discussions, the whole ﬂuid is superﬂuid and ρs = ρ, while the condensate density m|Ψ0 |2 is smaller than ρ because of the quantum depletion of the condensate. From a microscopic point of view, the link between BEC and the dynamic behaviour of superﬂuids has been the object of an extensive literature, based on the development of sophisiticated many-body approaches (see, for example, Griﬃn, 1993).

6.3

Hydrodynamic theory of superﬂuids: zero temperature

At zero temperature the equations which describe the macroscopic dynamics of superﬂuids have the classical form of irrotational hydrodynamics. In fact, in the absence of thermal excitations the macroscopic state of a superﬂuid can be described in terms of two variables, namely the density and the superﬂuid velocity. The equation for the mass density ρ = mn is given by the continuity equation ∂ρ + div(vs ρ) = 0, ∂t

(6.17)

expressing the conservation of mass. To derive the second equation we use the fact that, according to (6.15), the phase of the order parameter obeys the law ∂S 1 =− mvs2 + μ . (6.18) ∂t 2

Quantum hydrodynamics

71

As already mentioned in the previous section, it is natural to expect that this equation is valid not only at equilibrium, where both members are independent of position and time, but also when vs and ρ vary suﬃciently slowly in space and time. Taking the gradient of the equation for the phase and using expression (6.16) for the superﬂuid velocity, we ﬁnd the result m

m ∂vs +∇ v2s + μ(ρ) = 0, ∂t 2

(6.19)

where the chemical potential is evaluated locally by taking the value of a uniform ﬂuid at density ρ. Equation (6.19) has the same form as the Euler equation for the potential ﬂow of a nonviscous liquid. In the presence of an external potential Vext the chemical potential of eqn (6.19) should be replaced by μ(ρ) + Vext , and the equation for the velocity ﬁeld becomes m

m ∂vs +∇ v2s + μ(ρ) + Vext = 0. ∂t 2

(6.20)

A nontrivial solution of (6.20) is given by the equilibrium conﬁguration where vs = 0. In this case the density proﬁle satisﬁes the equation μ(ρ(r)) + Vext (r) = μ0 ,

(6.21)

which provides the ground state proﬁle in the so-called Thomas–Fermi approximation. In this equation μ0 ﬁxes the ground state value of the chemical potential in the presence of external trapping and is determined by the normalization condition drρ = N m. For dilute gases the hydrodynamic equations (6.17)–(6.20) can be derived explicitly starting from the time-dependent Gross-Pitaevskii equations and taking the Thomas–Fermi limit (see Section 5.2). In this case the chemical potential exhibits a linear dependence on the density and eqn (6.20) reduces to (5.23). The validity of the equations of hydrodynamics is, however, more general and also applies to strongly interacting superﬂuids, like helium, as well as to Fermi superﬂuids, where the dependence of the chemical potential on the density is very diﬀerent. Their applicability is always limited to the study of macroscopic phenomena.

6.4

Quantum hydrodynamics

According to equations (6.17)–(6.19) the small oscillations of the liquid are sound waves. In quantum mechanics these oscillations correspond to phonons, i.e. to the quanta of sound waves which can be described in the framework of a quantum scheme where the density and the velocity ﬁeld are replaced by proper operators. With respect to the traditional procedure of quantization of the classical ﬁeld described in Section 5.6, which is well suited for discussing dilute Bose gases, the quantization of the hydrodynamic equations has the advantage of also being applicable to highly correlated systems. An important application of the method is given by the Beliaev decay of phonons, a phenomenon experimentally observed in superﬂuid helium and which will be discussed in the next section.

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Superﬂuidity

In order to establish the commutation rules between the density and velocity ﬁeld operators it is convenient to derive the classical equations using the Hamilton formalism. The energy of the liquid, which will be denoted by H, can be presented in the form ρ 2 H= (∇φ) + e (ρ) dr, (6.22) 2 where we have introduced the velocity potential φ deﬁned by vs = ∇φ, while ρ is the density of the ﬂuid and e(ρ) is the internal energy per unit of volume. Since the chemical potential μ can be obtained from e(ρ) according to the law μ = mde/dρ, one gets, for the variation of H,

1 μ(ρ) 2 δH = −div (ρvs ) δφ + (∇φ) + δρ dr. (6.23) 2 m Thus the hydrodynamic equations (6.17)–(6.19) can be rewritten in the form δH ∂φ δH ∂ρ = , =− , ∂t δφ ∂t δρ which permits the identiﬁcation of the variables ρ and φ as the conjugate variables of the problem. This suggests that the quantization procedure is achieved by replacing these classical observables by operators satisfying the commutation rule (Landau, 1941) φˆ (r) ρˆ (r ) − ρˆ (r ) φˆ (r) = −iδ (r − r )

(6.24)

The quantization (6.24) transforms classical hydrodynamics into quantum hydrodynamics. Also, in the new scheme the phase S of the condensate, which ﬁxes the velocity potential through the relation (6.16), becomes an operator according to the relationship mˆ Sˆ = φ.

(6.25)

The quantum Hamiltonian can be obtained from (6.22) by choosing the proper symmetrized expression

ˆ = H

ρˆ ˆ ˆ ρ) dr . ∇φ ∇φ + e(ˆ 2

(6.26)

Quantum hydrodynamics, like any local quantum ﬁeld theory, exhibits ultraviolet divergencies. In our case these divergencies have a clear physical origin. In fact, we know that hydrodynamic theory is valid only in the macroscopic regime of small wave vectors. Despite these divergencies, the theory can be usefully employed to describe important phonon processes and to calculate the infrared behaviour of the relevant

Quantum hydrodynamics

73

correlation functions. This is particularly important in systems where Bogoliubov theory is not applicable, such as strongly correlated superﬂuids or in lower dimensions. Let us use the commutation relations (6.24) to express the operators ρˆ and φˆ in terms of the phonon annihilation and creation operators ˆb and ˆb† , respectively. For this purpose it is convenient to introduce the operators corresponding to the density change ρˆ = ρˆ − ρ¯, where ρ¯ is the constant density of the system (in this section we only consider uniform systems). The operator ρ can be presented in the form 1 ρˆ = √ Ak (ˆbk eik·r + ˆb†k e−ik·r ), 2V k=0

(6.27)

where V is the volume of the system and we have used a complete basis of plane wave functions. The operators ˆbk and ˆb†k are required to fulﬁl the usual Bose commutation relations ˆbk ˆb† − ˆb† ˆbk = δkk , k k

(6.28)

while the coeﬃcients Ak will be chosen in order to reduce the Hamiltonian in a diagonal ˆ The operator φ, ˆ which satisﬁes form, when expanded up to quadratic terms in ρˆ and φ. the commutation rule (6.24) with the density operator, is given by 1 −1 i (Ak ) (ˆbk eik·r − ˆb†k e−ik·r ). φˆ = − √ 2V k=0

(6.29)

This can easily be checked by using the identity V −1 k=0 eik·(r−r ) = δ (r − r ) , holding for large V . Let us expand (6.26) with to ρˆ . The linear term disappears because of the respect conservation of the mass ( drˆ ρ = 0). The next term, quadratic in the operators ρˆ ˆ and φ, is given by 1 c2 ρˆ2 (2) 2 ˆ dr, (6.30) ρ(∇φ) + H = 2 2 ρ¯ where c2 = (ρ/m) dμ/dρ is the square of the sound velocity. By substituting equations (6.27) and (6.29) into (6.30), one ﬁnds that (6.30) takes the diagonal form ωk ˆb†k ˆbk , (6.31) H (2) = k

which is typical of the Hamiltonian of independent phonons with dispersion ωk = ck, if one makes the choice 1/2 kρ Ak = , (6.32) c which ﬁxes the ﬁnal form of the operators φˆ and ρˆ in terms of the phonon operators b and b† . In deriving eqn (6.31) we have omitted a constant term originating

74

Superﬂuidity

from the noncommutativity of the operators b and b† . The diagonalization of the hydrodynamic Hamiltonian (6.26) in the form (6.31) has a close relation with the diagonalization of the Bogoliubov Hamiltonian made in Chapter 4 in the context of weakly interacting Bose gases. In particular, the occurrence of the infrared divergency in the velocity potential φˆ (see eqns (6.29) and (6.32)) is closely related to the one exhibited by the parameters u and v characterizing the Bogoliubov transformation (4.23). In Section 6.7 we will exploit the physical consequences of these divergencies which give rise to interesting features in the ﬂuctuations of the phase of the order parameter. The next term in the expansion of the Hamiltonian (6.26) describes the interaction between phonons. For example, processes involving three phonons are described by the third-order term 1 d c2 ρˆ (ˆ ρ)3 dr, (6.33) H (3) = ∇φˆ ∇φˆ + 2 6 dρ ρ which will be used in the next section to calculate the Beliaev damping associated with the decay of one phonon into two phonons.

6.5

Beliaev decay of phonons

In this section we apply the formalism of quantum hydrodynamics to discuss the problem of the disintegration of a phonon carrying momentum p into two phonons with momenta q and p − q respectively. This is a nonlinear process which can only be described by including the third-order term (6.33) in the Hamiltonian. Energy conservation gives the condition (p) = (q) + (|p − q|)

(6.34)

where (p) is the phonon dispersion law. For phonons with linear dispersion ( = up) this equation can only be satisﬁed if the momenta of all the three particles are parallel. Inclusion of the next term in the expansion (p) ≈ cp + αp3

(6.35)

for small p will generally yield a diﬀerent result. Infact, in this case eqn (6.34) takes the form c (p − q − |p − q|) = −α p3 − q 3 − |p − q|3 . At small p phonons are emitted at a small angle ϑ with respect to the direction of the initial phonon. On the left-hand side we have pq p − q − |p − q| ≈ − (1 − cos ϑ), (6.36) p−q while on right-hand side it is suﬃcient to put |p − q| ≈ (p − q). One then obtains the relationship 2

1 − cos ϑ = 3α (p − q) ,

(6.37)

which ﬁxes the value of the emission angle ϑ. This equation can only be satisﬁed if the coeﬃcient α is positive. In the opposite case the decay process cannot take place. For a

Beliaev decay of phonons

75

dilute Bose gas the coeﬃcient α is easily calculated using the Bogoliubov dispersion law (4.31) and is positive: α = (8m2 c)−1 . In superﬂuid 4 He α is positive at zero pressure (see Figure 8.5), but becomes negative at higher pressure. In order to calculate the probability of decay we must evaluate the matrix element of the third-order term (6.33) of the Hamiltonian. The terms in the operator ρˆ , responsible for the transition, are 1 ˆ ip·r/ ρˆ ∼ √ + Aqˆb†q e−iq·r/ + Ap−qˆb†p−q e−i(p−q)·r/ , Ap bp e 2V ˆ Substituting these operators in (6.33) and collecting terms with and analogously for φ. the combination ˆbpˆb†qˆb†p−q one obtains the result 1 (3) Hif = −i √ 2V

c pq(p − q) ρ

1/2 (6.38)

(3)

for the relevant matrix element Hif = p|H (3) |q, p − q. Result (6.38) holds for small values of p where the directions of p , q and p − q are practically the same. The probability per unit time for one phonon to decay into two phonons is given by the ‘golden rule’: w=

2π (3) 2 1 |Hif | δ (ε(p) − (q) − (|p − q|)), q 2

(6.39)

where the factor 1/2 accounts for the double counting of the phonon pairs with momentum q and p − q. By substituting the matrix element (6.38) and integrating over q one obtains the result 2 3 ρ2 d c2 w = p5 1 + . (6.40) 320πρ4 3c2 dρ ρ It is worth noticing that this probability does not depend on the explicit value of the parameter α, provided that this value is positive. The ﬁnite lifetime of the phonon implies that its energy possesses an imaginary part related to the decay probability by the relation Im (p) = − w/2. The factor 2 2 follows from the fact that the normalization integral |ψph | d3 x of the excitation depends quadratically on the phonon wave function and hence decays like e−2Imt/ . For a dilute Bose gas the quantity c2 is linear in the density so that the second term in the parentheses of the right-hand side of eqn (6.40) vanishes and the imaginary part of the phonon frequency becomes (Beliaev (1958)) γ ≡ −Im (p) =

3p5 . 640πρ3

(6.41)

The phonon decay discussed above is known in the literature as Beliaev decay. This decay mechanism can also be studied in nonuniform systems. Special care should be given in this case to the discreteness of the spectrum of elementary excitations.

76

6.6

Superﬂuidity

Two-ﬂuid hydrodynamics: ﬁrst and second sound

This section is devoted to the description of the dynamics of a superﬂuid at a ﬁnite temperature. We will consider situations where the free path of the elementary excitation is small compared to its wavelength and local thermodynamic equilibrium is ensured by collisions. In this case one can deﬁne the density and the temperature (or entropy) in every point of the ﬂuid. One has also to deﬁne the local superﬂuid and normal velocities. The general system of equations for these quantities was obtained by Landau (1941) (see also Landau and Lifshitz, 1987a). In the following we will limit ourselves to the description of the small-amplitude oscillations. The propagation of such oscillations at a ﬁnite temperature provides an important tool for investigating the consequences of superﬂuidity. First of all, the equation for vs has the same form (6.19) holding at zero temperature. Neglecting the term in v2s , we can write m

∂vs + ∇μ = 0, ∂t

(6.42)

where, at a ﬁnite temperature, one should take into account that the chemical potential μ depends not only on ρ, but also on T . The equation for the density has the usual form of the continuity equation: ∂ρ + div(mj) = 0, ∂t

(6.43)

where, according to eqn (6.7), the momentum density can be separated into the normal and superﬂuid components: mj = ρs vs + ρn vn ,

(6.44)

and the densities ρs and ρn can be taken equal to their equilibrium values. The time derivative of the momentum density mj is equal to the force per unit volume which in linear approximation is ﬁxed by the gradient of the pressure (we are here neglecting the presence of external ﬁelds). Thus we have the equation m

∂j + ∇P = 0. ∂t

(6.45)

The last equation is the equation for the entropy per unit volume s. This can be derived from general arguments. In fact if, dissipative processes such as viscosity and thermoconductivity are absent, the entropy is conserved and the equation for s takes the form of a continuity equation. Furthermore, only elementary excitations contribute to the entropy whose transport is hence ﬁxed by the normal velocity vn of the ﬂuid. The equation for the entropy per unit volume then takes the form ∂s + div(svn ) = 0, ∂t

(6.46)

where, in the linear regime, the entropy entering the second term should be taken at equilibrium.

Two-ﬂuid hydrodynamics: ﬁrst and second sound

77

The thermodynamic quantities entering the above equations are not independent and obey the Gibbs–Duhem thermodynamic equation ρdμ = −msdT + mdP.

(6.47)

It is also worth mentioning that this thermodynamic identity is valid only in the linear regime. In fact, in general the thermodynamic functions can also exhibit a dependence on the relative velocity vn − vs between the normal and the superﬂuid velocities. By excluding j from eqns (6.43) and (6.45) one obtains the important equation ∂2ρ = ∇2 P, ∂t2

(6.48)

relating the time and space variations of the density and of the pressure, respectively. Our purpose now is to derive an equation relating the time and space variations of the temperature and of the entropy. To achieve this it is convenient to rewrite eqn (6.46) in terms of the entropy per unit mass s = s/ρ. Using the equation of continuity (6.43) one can write ∂ s sρs + div(vn − vs ) = 0 . ∂t ρ

(6.49)

On the other hand, using the thermodynamic relation (6.47) and eqns (6.42) and (6.45), one ﬁnds ρn

∂ (vn − vs ) + ρ s∇T = 0, ∂t

(6.50)

which, combined with eqn (6.49) yields the required equation ∂ 2 s ρs s2 2 = ∇ T. ∂t2 ρn

(6.51)

By using the relationships δρ =

∂ρ ∂ s ∂ s ∂ρ δP + δT , δ s= δp + δT ∂P ∂T ∂p ∂T

(6.52)

one ﬁnds that equations (6.48) and (6.51) provide coupled equations for the pressure and the temperature. By looking for plane wave solutions varying in time and space like e−iω(t−x/c) , one then obtains the following equation for the velocity of sound:

∂ s ∂ρ ∂ s ∂ρ 4 ρs s2 ∂ρ 2 ρs s2 ∂ s − c − + c + = 0, (6.53) ∂T ∂P ∂P ∂T ∂T ρn ∂P ρn where the derivatives with respect to T are taken at constant pressure and vice versa. A lengthy but straightforward calculation, based on standard thermodynamic relations, permits us to rewrite equation (6.53) in the more convenient form (Landau, 1941)

∂P ρs T s2 2 ρs T s2 ∂P c4 − c + + = 0, (6.54) ∂ρ s ρn c˜v ρn c˜v ∂ρ T

78

Superﬂuidity

where c˜v = T (∂ s˜/∂T )ρ is the speciﬁc heat at constant volume per unit mass and the derivative at constant s˜ corresponds to an isoentropic transformation since the quantity N m˜ s coincides with the entropy of the system. Equation (6.54) gives rise to two distinct sound velocities if ρs = 0. This is the consequence of the fact that in a superﬂuid there are two degrees of freedom associated with the normal and superﬂuid components. The existence of two types of sound waves in a Bose–Einstein condensed system was ﬁrst noted by Tisza (1940). Equation (6.54) is easily solved as T → Tc , i.e. close to the transition temperature where ρs → 0. In this case the upper solution (ﬁrst sound) is given by the isoentropic velocity ∂P c21 = , (6.55) ∂ρ s and exhibits a continuous transition to the usual sound velocity above Tc . In the same limit the lower solution (second sound) takes the form c22 =

ρs T s2 , ρn C˜p

(6.56)

and identically vanishes at the transition where ρs = 0. In the above equation we have introduced the speciﬁc heat at constant pressure, related to C˜v by the thermodynamic relation C˜p /C˜v = (∂P/∂ρ)s˜/(∂P/∂ρ)T˜ . Results (6.55) and (6.56) hold also in the T → 0 limit where one can set (∂P/∂ρ)T = (∂P/∂ρ)s and C˜P = C˜v . In this limit all the thermodynamic functions as well as the normal density ρn are ﬁxed by the thermal excitation of phonons and eqn (6.56) yields result c22 = c21 /3 for the second sound velocity. For systems characterized by a small thermal expansion coeﬃcient (and hence almost equal values of the isothermal and adiabatic compressibilities), eqn (6.56) provides an excellent approximation to the second sound velocity in the entire superﬂuid region 0 < T < Tc . These systems include the celebrated superﬂuid 4 He and the interacting Fermi gas at unitarity (see Section 16.6). Equation (6.56) points out explicitly the crucial role played by the superﬂuid density and was actually employed to determine the temperature dependence of the superﬂuid density in liquid 4 He in a wide interval of temperatures (Dash and Taylor, 1957). However, eqns (6.55) and (6.56) are inadequate to describe the sound velocities in dilute Bose gases at intermediate values of T , due to the high isothermal compressibility exhibited by these systems. A simple description is obtained by noticing that, for temperatures kB T μ = gn, all the thermodynamic functions of the weakly interacting Bose gas, except the isothermal compressibility, can be safely evaluated using the ideal Bose gas model. This simpliﬁes signiﬁcantly the calculation of eqn (6.54). In fact, in the ideal Bose gas model one ﬁnds the simple result

∂P ∂ρ

+ s

ρs T s2 ρT s˜2 = ˜ ρn Cv ρn C˜v

(6.57)

Two-ﬂuid hydrodynamics: ﬁrst and second sound

79

for the coeﬃcient of the c2 term. It is now easy to derive the two solutions satisfying the condition c1 c2 . To obtain the larger velocity c1 one can neglect the last term in (6.54). Using the thermodynamic relations of the ideal Bose gas model (see Section 3.2) and identifying the normal density with the thermal density (ρn = mnT = mNT /V ) one obtains the prediction c21 =

5 g5/2 kB T 3 g3/2 m

(6.58)

for the ﬁrst sound velocity (Lee and Yang, 1959). Corrections to c21 due to the interaction have been calculated by Griﬃn and Zaremba (1997). As T → Tc this branch approaches the usual sound velocity of an ideal Bose gas above Tc . To calculate c2 we must instead neglect the c4 term in (6.54), and using result (6.57) one ﬁnds ρs ∂P 2 c2 = . (6.59) ρ ∂ρ T To a ﬁrst approximation the inverse isothermal compressibility ρ (∂P/∂ρ)T of a weakly interacting Bose gas, except near the critical temperature, is equal to its zero-temperature value gρ2 /m2 . This result can easily be understood working in the Hartree–Fock approximation (see Section 13.2) which yields the result μ = g (n + nT ) for the chemical potential where nT is the thermal density. Using the thermodynamic identity (∂P/∂ρ)T = n (∂μ/∂ρ)T and noting that in ﬁrst approximation nT is independent of the density, we obtain the result (∂P/∂ρ)T = gn/m which permits us to rewrite the second sound velocity as c22 =

gn0 (T ) , m

(6.60)

where, consistently with the approximation made above, we have set ρs (T ) = mn0 (T ) = mN0 (T )/V . At temperatures much smaller than Tc (where n0 (T ) ∼ n), but still large compared to μ/kB T , result (6.60) approaches the T = 0 Bogoliubov sound velocity (4.15). This is a clear signature of a hybridization between the ﬁrst and second sound modes which is schematically illustrated in Figure 6.1. The occurrence of this hybridization was ﬁrst identiﬁed in the seminal work by Lee and Yang (1959). In order to obtain the results for c21 and c22 in the intermediate region kB T ∼ μ one should calculate the thermodynamic functions using the Bogoliubov spectrum of elementary excitations. This region is conveniently described by introducing the dimensionless variables t˜ = kB T /gn and η = gn/kB Tc where Tc is the critical temperature of the ideal Bose gas. Bogoliubov theory provides the correct thermodynamic functions provided T Tc , i.e. t˜ η −1 . The hybridization region t˜ ∼ 1 is consequently compatible with the use of Bogoliubov theory provided η 1 and hence T Tc . In this range of temperatures one can safely use the T = 0 Bogoliubov spectrum of elementary excitations to calculate

80

Superﬂuidity

3

2

c1

1

c2

0

0

0.25

0.5 T /Tc

0.75

1

Figure 6.1 Schematic representation of the velocity of ﬁrst and second sound in a dilute Bose gas as a function of temperature in units of the T = 0 Bogoliubov velocity gn/m. The ﬁgure points out the eﬀect of hybridization between the two modes taking place at low temperature. Above Tc only the ﬁrst sound survives.

the thermodynamic functions. For the free energy one ﬁnds the following expression (Verney et al., 2015) ∞ √ 2 E0 2t˜ A ˜ 3/2 √ η = + p (6.61) p˜2 ln 1 − e−˜p p˜ +4/2t d˜ gnN gnN ζ(3/2) 2π 0 in terms of t˜ and η, from which all the thermodynamic functions can be easily calculated. E0 is here the ground state energy. The normal density, using the Landau’s deﬁnition (6.10), instead takes the form √ ∞ 4 p˜ p˜2 +4/2t˜ ρn p ˜ e 2 √ η 3/2 = p. (6.62) √ 2 d˜ 2 ρ ˜ 3ζ(3/2)t˜ 2π 0 ep˜ p˜ +4/2t − 1 The idea now is to calculate the two solutions of (6.54) for a ﬁxed value of t˜ of the order of unity, taking the limit η → 0. Physically this corresponds to considering very low temperatures (of the order of μ) and very small values of the gas parameter na3 ∼ η 3 . By writing the solutions of eqn (6.54) in terms of the T = 0 Bogoliubov sound velocity cB = gn/m, one ﬁnds that in the η → 0 limit the two sound velocities only depend on the dimensionless parameter t˜ and are given by c2+ = c2B c2− (t˜) = c2B f (t˜),

(6.63)

where f (t˜) is a dimensionless function determined by mρT s˜2 . f (t˜) = limη→0 ρn c˜v gn

(6.64)

Fluctuations of the phase

81

The two velocities coincide (hybridization point) for t˜ = t˜cr ∼ 0.6. At lower temperatures c2− approaches, as expected, the zero temperature value c2B /3. Inclusion of ﬁnite, although small, values of η causes the appearance of a gap between the two branches at the hybridization point, proportional to η 3/4 . The mechanism of hybridization permits the identiﬁcation of an upper branch c1 (which coincides with c+ for t˜ < t˜cr and with c− for t˜ > t˜cr ) and a lower branch c2 (which instead coincides with c− for t˜ < t˜cr and with c+ for t˜ > t˜cr ). The above discussion explains why, for temperatures larger than μ/kB , the lower branch (second sound) physically coincides with the oscillation of the condensate, sharing the same physical behaviour of the T = 0 sound mode predicted by Bogoliubov theory. This behavior has been conﬁrmed experimentally by Meppelink et al. (2009). The results illustrated in this section are valid if all the thermodynamic quantities vary slowly over distances of the order of the mean free path of the elementary excitations. This condition is rather severe at low temperatures where collisions are rare. In this respect an alternative regime that one should investigate is the collisionless regime, which is particularly important at low temperatures (see Section 13.7).

6.7

Fluctuations of the phase

By developing the formalism of hydrodynamics in Section 6.4 we have derived the explicit form for the density and the velocity potential operators in terms of the phonon creation and annihilation operators ˆb† and ˆb (see eqns (6.27) and (6.29)). These results permit us to calculate the ﬂuctuations of the density as well as of the phase of the condensate. In fact, the phase of the order parameter is related to the velocity potential by the relation (6.25). By using result (6.32) the density and phase operators take the following form, holding at low temperature where ρs ∼ ρ: 1/2 1 ρk (ˆbk eik·r + ˆb†k e−ik·r ), ρˆ = √ c 2V k

(6.65)

1/2 1 mc μt ˆ √ (ˆbk eik·r − ˆb†k e−ik·r ) − i S=− ρk 2V k

(6.66)

and

which explicitly show that the Fourier components of the phase operators become increasingly large as k → 0. It is worth noticing that the kinetic energy term depends on the square of the gradient of the phase, so that the infrared divergency of the phase does not result in any peculiar eﬀect in the energy. Other physical quantities, like the long-range behaviour of the one-body density matrix, are instead strongly aﬀected by this divergency, as we will discuss below. ˆ † (r)Ψ(r ˆ ) can be calculated in the The one-body density matrix n(1) (r, r ) = Ψ long-range limit using the following macroscopic representation of the ﬁeld operator: ˆ (r, t) = √n0 eiSˆ , Ψ

(6.67)

82

Superﬂuidity

where n0 is the condensate density and Sˆ is the phase operator for which we will use the hydrodynamic expression (6.66). In writing (6.67) we have used the fact that the operatorial nature of n0 can be ignored for calculating the one-body matrix at large distances where the leading eﬀects are given by the ﬂuctuations of the phase. By using the fact that the probability distribution for the occurrence of phase ﬂuctuations is Gaussian, the one-body density matrix can be written in the form ˆ ˆ ˆ ˆ 2 n(1) (r, r ) = n0 e−i(S(r)−S(r )) = n0 e− (S(r)−S(r )) /2 = n0 e−(χ(0)−χ(s)) , (6.68) where we have deﬁned the phase correlation function χ(s) = S(r)S(r )

(6.69)

and s = |r − r |. The relation (6.68) between the one-body density matrix and the phase correlation function holds at both zero and a ﬁnite temperature. By expanding the exponent up to terms linear in the phase correlation function we ﬁnd n(1) (s) ≈ n0 e−χ(0) (1 + χ(s)).

(6.70)

Notice that, in contrast to the one-body density matrix, the phase correlation function is not gauge invariant. In carrying out the expansion (6.69) we have assumed that χ vanishes when s → ∞ (this can always be imposed by a proper choice of the absolute value of the phase). According to the general deﬁnition (2.10), the quantity n0 e−χ(0) provides the renormalized value of the condensate fraction which diﬀers from unity even at T = 0 because of quantum depletion (in the following this renormalized value will still be indicated with n0 ). Using result (6.66) for the phase operator the function χ takes, for low temperatures, the form m2 c 1 eip·s/ dp χ (s) = Np + , (6.71) ρ 2 p (2π)3 ! where s = |r − r |, p = k and Np = ˆb†pˆbp = ecp/kB T − 1 is the thermal distribution of phonons. The Fourier transform of (6.69) permits us to calculate the particle occupation number (see eqns (2.5) and (2.17)), for which we obtain the result n0 mc 1 np = Np + (6.72) np 2 at small p. At zero temperature, where Np = 0 one ﬁnds the divergent behaviour (Gavoret and Nozi`eres, 1964) np =

n0 mc 2np

(6.73)

at small p, giving rise to the asymptotic behaviour n(1) (s) = n0 + n0

mc s2 4π 2

(6.74)

Fluctuations of the phase

83

for large s. Results (6.73) and (6.74) agree with eqns (4.46) and (4.51) which were derived for a dilute gas where n0 ≈ n. At ﬁnite temperatures one instead ﬁnds, for cp kB T , np =

n0 mkB T np2

(6.75)

(Hohenberg and Martin, 1965). Also this equation is in agreement with result (4.52) derived for a dilute gas. Equation (6.72) permits the calculation of the thermal depletion of the condensate. In fact, the direct integration of the momentum distribution for the particle with p = 0 yields the following result (Ferrell et al., 1968): 2 n0 (T ) − n0 (0) mc m (kB T ) Np dp =− = − , (6.76) n0 (0) n p (2π)3 12nc3 which was already derived in Chapter 4 for a weakly interacting Bose gas (see eqn (4.54)). It is worth noticing that the quantum depletion at zero temperature can not be calculated by this method, since the corresponding integral contains an ultraviolet divergency. The thermal ﬂuctuations of the phase can be calculated not only at low temperatures where ρs ∼ ρ but also for higher temperatures up to the transition point, starting from the expression 1 1 Ekin = dr ρs v2s + ρn v2n (6.77) 2 2 for the kinetic energy. To this purpose it is convenient to write the phase of the order parameter in the form 1 S (r) = Sk eik·r , (6.78) V k

so that, using the expression vs = /m∇S for the superﬂuid velocity, the superﬂuid contribution to (6.77) can be written as 2 1 ρs 1 2 2 ρs vs dr = k |Sk |2 . (6.79) 2 m 2 V k

This equation implies that the probability P (Sk ) of generating a ﬂuctuation of the phase with Fourier component Sk is given by

2 ρs k 2 |Sk |2 P (Sk ) = e−δE/kT = exp − 2 , (6.80) 2m kB T V and the corresponding average of |Sk |2 takes the value |Sk |2 kB T m 2 = 2 2 . V k ρs

(6.81)

84

Superﬂuidity

By using the relationship S(r)S(r ) =

1 ik·s |Sk |2 e V V

(6.82)

k

and result (6.81) one can evaluate the long-range behaviour of the one-body density matrix (6.68). One ﬁnds kB T m2 (1) n (s)s→∞ = n0 1 + (6.83) s4π2 ρs or, equivalently, the particle occupation number (np )p→0 =

kB T n0 m2 , p2 ρs

(6.84)

where p = k. This equation generalizes result (6.75) to higher temperatures where ρs = ρ and is even valid near the transition point where both n0 and ρs tend to zero. However, the condition of applicability near the transition point becomes severe since the healing length is very large and the applicability of the hydrodynamic approach is restricted to extremely small values of p. Let us conclude this session by discussing the behaviour of the thermal ﬂuctuations of the velocity ﬁeld. Equation (6.81) permits us to calculate directly the ﬂuctuations of the superﬂuid velocity vs . In fact, deﬁning the Fourier component of the velocity ﬁeld according to v = (1/V ) k (vk ) eik·r , one ﬁnds that the Fourier transform of the superﬂuid velocity is given by ikSk /m, and hence (vsk ) (vsk )∗m =

kB T k km V. k 2 ρs

(6.85)

The ﬂuctuations of the normal velocity vn can instead be calculated directly from the contribution of the normal component to the kinetic energy (6.77). They are given by (vnk ) (vnk )∗m =

kB T δm V ρn

(6.86)

and exhibit a diﬀerent tensorial structure with respect to (6.85). The diﬀerence is the consequence of the irrotationality constraint obeyed by the superﬂuid velocity ﬁeld. Using expression (6.7) for the current one can ﬁnally obtain the following result for the ﬂuctuations of the k-th component of the current: (jk ) (jk )∗m =

ρ s kB T ρn k km V + 2 kB T δm V. m2 k 2 m

(6.87)

This relationship holds in the regime of ‘high’ temperatures kB T (p) where is the energy of the elementary excitations and p = k. Under these conditions the ﬂuctuations of the phase are dominated by thermal eﬀects and one can safely ignore the quantum ﬂuctuations which only become important at lower temperatures.

Rotation of superﬂuids

6.8

85

Rotation of superﬂuids

We have already mentioned that a superﬂuid cannot rotate as an ordinary liquid. If the liquid is enclosed in a cylindrical container rotating around its axis of symmetry, only the normal component will be brought into rotation. At a low enough angular velocity the superﬂuid part will instead remain at rest. However, for a suﬃciently large angular velocity such a state becomes energetically unfavourable. The reason is that, in the frame rotating with the angular velocity of the container where thermal equilibrium is expected to take place, the physical quantity to minimize is Er = E − Ω · L,

(6.88)

where E and L are, respectively, the energy and angular momentum in the coordinate frame of the laboratory and Ω is the angular velocity of the container. From eqn (6.88) one can deduce that, for suﬃciently large Ω, states with Ω · L > 0 will be thermodynamically more favourable than the state with L = 0, corresponding to the superﬂuid at rest. Since a superﬂuid cannot rotate in a rigid way the rotation will eventually be realized through the creation of quantized vortex lines. In Section 5.3 we investigated such conﬁgurations in a dilute Bose gas. In this section we provide a generalization to arbitrary superﬂuids. Let us ﬁrst calculate the circulation of the superﬂuid velocity around such a line. The superﬂuid velocity can be expressed by equation (6.16) in terms of the phase S of the condensate wave function. This implies that the circulation takes the form vs · dl = ∇S · dl = 2π s, (6.89) m m where s should be an integer in order to ensure that the wave function be single valued. This implies that the circulation is quantized in units of h/m. Let us consider a single straight vortex line along the symmetry axis of a cylindrical vessel. In this case the streamlines of vs are circles lying on planes perpendicular to the symmetry axis, and from equation (6.89) one has vs = s

, mr

(6.90)

where r is the distance from the line. This law should be compared with the velocity ﬁeld v = Ωr associated with a rigid rotation. The angular momentum Lz of the ﬂuid is easily calculated and is given by Lz = ρs vs rdr = πR2 Lsρs , (6.91) m where L is the length of the vessel and R its radius. In deriving the last equality we have assumed that the size rc of the vortex core, characterizing the region where the superﬂuid density is signiﬁcantly perturbed, is small compared to R, and ρs is the value of the superﬂuid density far from the core.

86

Superﬂuidity

The energy associated with the vortex line is dominated by the kinetic energy term. A simple calculation yields Ev =

1 ρs vs2 dr = Lπρs s2 2

m

2

ln

R , rc

(6.92)

where the integration with respect to the radial variable has been taken between the size rc of the vortex core and the radius R of the sample. In the case of superﬂuid helium the size of the core is of the order of the interatomic distance, while in a dilute gas it is ﬁxed by the healing length (rc = ξ/1.46). Notice, however, that the dependence of (6.92) on rc is logarithmic and hence the energy of the vortex depends very weakly on the actual value of the core size. Equations (6.91) and (6.92) also explain why vortices with |s| > 1 are energetically unstable. This follows from the fact that the energy Ev scales like s2 while Lz increases linearly with s. Using result (6.92) we can easily ﬁnd the critical value Ωc for the existence of an energetically stable vortex line. This value is obtained by imposing that the change in the energy Er (6.88) due to the creation of the vortex be equal to Ev . Using (6.91) and (6.92) we ﬁnd Ev R Ωc = (6.93) = ln Lz mR2 rc for vortices with a single quantum of circulation, s = 1 (Feynman, 1954). It is worth stressing that vortex lines can exist as a stationary conﬁguration only in a superﬂuid. In fact, even in the presence of an small shear viscosity, the vorticity curlvs = 2π

(2) δ (r⊥ )ˆz, m

(6.94)

characterizing the vortex will diﬀuse from the z-axis and will eventually spread over the whole volume of the vessel resulting in a solid-like rotation. It follows that the existence of quantized vortex lines can be considered a proof of the absence of viscosity and consequently of superﬂuidity. If one considers angular velocities signiﬁcantly larger than Ωc then more vortices will appear in the ﬂuid. For very large Ω the rotation of the system will then look similar to the one of a rigid body characterized by the law curlvs = 2Ω. Using result (6.94) ˆ, one ﬁnds that the average vorticity per unit area is given by curlvs = (h/m)nv z where nv is the number of vortices per unit area, so that the density of vortices is related to the angular velocity Ω by the relation nv =

m Ω. π

(6.95)

Equation (6.95) can be used to evaluate the maximum number of vortices that can be hosted in a given area as a function of the angular velocity. At a ﬁnite temperature the presence of vortices changes the properties of a superﬂuid in a substantial way. A vortex line is at rest with respect to the superﬂuid and

Rotation of superﬂuids

87

actually represents a defect. Elementary excitations of the normal part can scatter on it, transferring momentum. As a result, in the presence of a relative motion vs − vn in the plane perpendicular to the line, such collisions give rise to a mutual friction force between the normal and the superﬂuid components, causing energy dissipation. This implies that, in the presence of vortex lines, the equilibrium distribution (6.6) of elementary excitations cannot be achieved, unless vs = vn . The concept of mutual friction was introduced empirically by Gorter and Mellink (1949) and measured in rotating superﬂuid 4 He by Hall and Vinen (1956). The vortex conﬁgurations discussed above correspond to a uniform rotation of the system. Diﬀerent rotational motions can occur if the vortex lines have a more complicated form. As in the case of a dilute gas one can generate, for example, vortex rings whose macroscopic description, presented in the ﬁrst part of Section 5.4, also holds for a generic superﬂuid. In the following we will discuss the behaviour of the longwave oscillations of a slightly deformed vortex line. In these oscillations the vortex line takes the form of a rotating spiral. The coordinates of the line can be represented as x = d cos(kz − ωt) , y = d sin(kx − ωt)

(6.96)

and correspond to a wave of length λ2π/k propagating along the z-th axis. The value of the angular velocity ω ﬁxes the precession of the spiral and can be calculated from the knowledge of the energy and of the angular momentum carried by the spiral vortical line. The kinetic energy (1/2) ρs vs2 dr associated with the deformed line should be calculated starting from the expression v = (/2m) dl × r/r 3 for the velocity ﬁeld, where dl is an element of the line. The problem is equivalent to the calculation of the magnetic energy associated with a curved wire carrying a stationary current, the superﬂuid velocity ﬁeld playing the role of the magnetic ﬁeld. Within logarithmic accuracy the energy can be obtained starting from result (6.92) derived for a straight line. The length L entering eqn (6.92) becomes the length of the deformed line and is given by the simple expression 2 2 1 ∂x ∂y L= (6.97) 1+ + dz L0 1 + d2 k 2 , ∂z ∂z 2 where L0 is the length of the line at rest. In the following we will consider oscillations satisfying the condition λ = 2π/k R, where R is the radial size of the sample. In this case the region of space contributing to the energy change caused by the deformation extends up to radial distances of the order of λ. In fact, for larger distances the changes in the velocity ﬁeld vanish rapidly and the spiral behaves like a straight line. In conclusion, the energy change due to the deformation is given by the simple law 2 π 1 δEv = L0 d2 ρs , (6.98) k 2 ln 2 m k˜ rc where the actual value of r˜c is sensitive to both the short-range cut-oﬀ ﬁxed by the size of the vortex core as well as to the long-range cut-oﬀ of the order of the wavelength of

88

Superﬂuidity

the oscillation. If λ is comparable to or larger than the radial size, the radial integration needed to calculate δEv extends up to R and in this case the value of δEv would depend explicitly on the radial size of the sample. Let us now calculate the angular momentum of the spiral. This calculation is simpliﬁed by the fact that, in the limit of large wavelengths, the result is independent of k and can consequently be derived by considering a straight vortex line displaced from the z-th axis by the distance d. By writing the integral (6.91) in cylindrical coordinates r, ϕ, and z with respect to the axis of the cylinder, i.e. with respect to the axis of the vortical line at rest, one ﬁnds Lz = ρs L0 rdr⊥ dϕrvϕ = ρs L0 rdr v · dl , (6.99) " where the countour of the integration corresponds to a circle of radius r. The corresponding integral vanishes if r < d since"in this case the circuit does not enclose the vortex line. Conversely for r > d one has v · dl = 2π/m. In conclusion, one simply ﬁnds the result δLz = −πd2 L0 ρs

, m

(6.100)

showing that the deformation of the vortex line always reduces the value of angular momentum. The angular velocity of the precession can now be calculated using the general equation ω = ∂Ev /∂Lz . One ﬁnds 2 ∂Ev /∂d 1 =− k ln ω= , (6.101) ∂Lz /∂d 2m krc and this turns out to be negative. This means that the spiral rotates in a direction opposite to the rotation of the liquid. The dispersion law (6.101) was ﬁrst derived by Lord Kelvin, who studied the small oscillations (Kelvin waves) of a classical vortex (Thomson, 1880). In a dilute Bose gas it is possible to calculate the exact value of r˜c by solving the Gross-Pitaevskii equation. The result is that the value of r˜c practically coincides with the healing length (Roberts, 2001 and 2003). The harmonic oscillations of the vortex line discussed above can be naturally quantized. This provides an interesting class of elementary excitations exhibited by superﬂuids in the presence of a vortex line. In the quantum picture each excitation has energy |ω|. By comparing eqn (6.101) with (6.98) one ﬁnds that the value of d2 associated with a single quantum of excitation is ﬁxed by the relation πd2 L0 ρs /m = 1. According to (6.100) this implies that the angular momentum carried by each quantum of excitation is given by (−).

7 Linear Response Function Linear response theory is a powerful tool with which to explore the dynamic behaviour of interacting many-body systems at zero temperature as well as at ﬁnite temperatures. It can be employed to obtain valuable information both on the collective behaviour, which characterizes the macroscopic excitations of the system, and on the momentum distribution, which determines the response at high-momentum transfer where the external probe scatters incoherently from the individual constituents. In Bose–Einstein condensed systems both the collective excitations and the momentum distribution exhibit peculiar features which are worth discussing. In this chapter we present a general discussion of the formalism by introducing the concepts of dynamic polarizability, dynamic structure factor, and sum rules. Special emphasis will be given to density excitations, but the response to a current ﬁeld will also be considered in order to provide a link with the theory of superﬂuidity. We will also derive general inequalities, based on the formalism of linear response theory, which provide useful bounds for the excitation energies as well as for the ﬂuctuations of physical observables. In the last part of this chapter the formalism will be explicitly illustrated in the case of the ideal and weakly interacting Bose gas.

7.1

Dynamic structure factor and sum rules

Let us consider a many-body system described by the Hamiltonian H, and let F and G be two linear operators of physical interest. Without any signiﬁcant loss of generality we may assume that at equilibrium the average values of these operators are vanishing. The linear response function, also called dynamic polarizability, provides the ﬂuctuation δF † generated by an external ﬁeld coupled to the system through the time-dependent Hamiltonian Hpert (t) = −λGe−iωt eηt − λ∗ G† e+iωt eηt .

(7.1)

In eqn (7.1) λ is the strength of the external ﬁeld that will be taken to be suﬃciently small in order to apply linear response theory. The presence of the factor eηt , with η positive and small, ensures that at t = −∞ the system is governed by the unperturbed Hamiltonian H. The adiabatic condition implied by this factor is crucial in order to work in the linear regime. The ﬂuctuation δF † induced by the perturbation oscillates with the same frequency ω as the external ﬁeld (7.1). The dynamic polarizability χF † ,G is deﬁned by the relation δF † = λe−iωt eηt χF † ,G (ω) + λ∗ e+iωt eηt χF † ,G† (−ω)

(7.2)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

90

Linear Response Function

and satisﬁes the property χ∗F † ,G (ω) = χF,G† (−ω). The function χF † ,G (ω) depends only on the properties of the system in the absence of the external probe and can be straightforwardly calculated using perturbation theory. Let us suppose that at t = −∞ the system is in thermal equilibrium at temperature T . One then ﬁnds the result (Kubo, 1956, 1957)

1 −1 −βEm m|F † |nn|G|m m|G|nn|F † |m χF † ,G (ω) = − Q − , (7.3) e ω − ωnm + iη ω + ωnm + iη m,n where |n and ωnm = (En − Em )/ are the eigenstates and the transition frequencies relative to the unperturbed Hamiltonian (H|n = En |n), while Q = m exp(−βEm ) is the partition function. The Boltzmann factor exp(−βEn ) accounts for the thermal equilibrium of the initial conﬁguration. If the excitation operators do not conserve the total number of particles then it is convenient to use the grand canonical formalism and to replace En with En − μN . A useful quantity is the dynamic structure factor relative to the operator F : SF (ω) = Q−1 e−βEm |n|F |m|2 δ(ω − ωnm ), (7.4) m,n

which reduces to SF (ω) =

|n|F |0|2 δ(ω − ωn0 )

(7.5)

n

at zero temperature, where only the ground state |0 contributes to the sum m of eqn (7.4). Equation (7.5) shows that at T = 0 the dynamic structure factor identically vanishes for ω < 0. In fact, the excitation energies ωn0 are always positive, the system being in its ground state. At ﬁnite temperatures the dynamic structure factor obeys the important relation SF (ω) = eβω SF † (−ω),

(7.6)

which follows from (7.4) by interchanging the indices m and n in the sum. This relationship expresses the principle of detailed balancing, stating that the probabilities (proportional to SF (ω) and SF † (−ω), respectively) that the system absorbs and releases energy, as a consequence of the coupling with the external perturbation, are related each other by the Boltzmann factor eβω . In the following we will consider the simplest case in which the two operators F and G coincide: F = G. In terms of the dynamic structure factor SF the corresponding response function χF ≡ χF † ,F can be written as

+∞ SF † (ω ) SF (ω ) − . (7.7) χF (ω) = − dω ω − ω + iη ω + ω + iη −∞ Using the Dirac relation lim

η→0

1 1 =P − iπδ(x − a), x − a + iη x−a

(7.8)

Dynamic structure factor and sum rules

91

where P is the principal part, the function χ can be naturally separated into its real and imaginary parts: χF (ω) = χF (ω) + iχF (ω).

(7.9)

From eqn (7.7) one then obtains the relations χF (ω) = −

+∞

−∞

dω SF (ω )P

1 1 − SF† (ω )P ω − ω ω + ω

(7.10)

and χF (ω) = π(SF (ω) − SF † (−ω)),

(7.11)

which show that the functions χ and χ are, respectively, even and odd with respect to change of ω and F into −ω and F † . Using the detailed balancing relation (7.6), eqn (7.11) can also be rewritten in the useful form χF (ω) = π(1 − e−βω )SF (ω).

(7.12)

The function χ is also called the dissipative component of the response function. In fact, using second-order perturbation theory, the energy transfer per unit time from the external ﬁeld (7.1) to the system can be written as (F = G) dE = 2|λ|2 ωχF (ω) dt

(7.13)

plus terms oscillating at the frequency 2ω, corresponding to reversible deformations of the system. By means of (7.11) one can also write dE = 2π|λ|2 ω(SF (ω) − SF † (−ω)), dt

(7.14)

showing that the energy rate is given by the diﬀerence of two terms. The former corresponds to the probability for the perturbation to transfer energy ω to the system, while the latter gives the probability to extract energy ω from the system. Both processes are induced by the external perturbation (7.1) with F = G. Notice that, if the system is in thermal equilibrium and hence relation (7.12) holds, the total rate dE/dt is always positive. The above considerations are particularly important at ﬁnite temperatures. In fact, while at T = 0 χF (ω) and SF (ω) coincide for positive ω and only processes transferring energy to the system are allowed, at ﬁnite temperatures the two functions diﬀer signiﬁcantly if βω is small. In general, the dynamic structure factor exhibits a much stronger dependence on T with respect to χ , which consequently represents a more fundamental quantity from the point of view of many-body theory.

92

Linear Response Function

Im (ω’)

C

ω

Re (ω’)

Figure 7.1 Integration contour used to derive the Kramers–Kronig relations.

Let us brieﬂy recall the analytic properties of the response function χF . We consider the integral χF (ω ) dω = 0 (7.15) C ω−ω in the ω -complex plane where the contour C is indicated in Figure 7.1. The integral vanishes because, as a consequence of the factor eηt in the external perturbation (7.32), the poles of the response function lie in the lower half of the complex plane. Since the response function vanishes at least as rapidly as 1/ω for large ω (see eqn (7.23) below), the contributions to (7.15) arise from the integral along the real axis (principal part) and from the integral on the half circle surrounding the point ω. By separating in χ the real and imaginary parts one ﬁnally obtains the Kramers–Kronig relations (Kronig, 1926; Kramers, 1927) χF (ω) = −

1 π

+∞

−∞

1 ω − ω

(7.16)

1 , ω − ω

(7.17)

dω χF (ω )P

and χF (ω) =

1 π

+∞

−∞

dω χF (ω )P

which express the causal nature of the response to the perturbation. The explicit determination of the response function or, equivalently, of the dynamic structure factor requires in general the full solution of the Schr¨ odinger equation, yielding the eigenenergies and matrix elements of eqn (7.3). Useful information on the behaviour of the dynamic structure factor is given by the method of sum rules, which provide an algebraic way to evaluate the moments of the dynamic structure factor mp (F ) = p+1

+∞

−∞

dωω p SF (ω).

(7.18)

Dynamic structure factor and sum rules

93

Using the completeness relation n |nn| = 1 and deﬁnition (7.4) for the dynamic structure factor, one easily obtains the following exact identities: m0 (F ) + m0 (F † ) = {F † , F },

(7.19)

m0 (F ) − m0 (F † ) = [F † , F ],

(7.20)

m1 (F ) + m1 (F † ) = [F † , [H, F ]], and

(7.21)

m1 (F ) − m1 (F † ) = {F † , [H, F ]},

(7.22)

where we have considered only the lowest moments. In general, SF = SF † so that also the sum rules (7.20) and (7.22) may diﬀer from zero. The sum rules (7.20) and (7.21) characterize the high-frequency expansion of the dynamic response function, which takes the form χF (ω)ω→∞ = −

1 1 [F † , F ] − [F † , [H, F ]], ω (ω)2

(7.23)

showing that the leading term in the high-frequency expansion behaves in general as 1/ω. This term vanishes in the case of the density response function since the density operator commutes with its adjoint. Equation (7.23) also shows that the sum rules (7.19) and (7.22) containing the anticommutators do not enter the above expansion. In the opposite limit of small ω the dynamic polarizability approaches its static limit (static polarizability) according to the law χF (0) ≡ χF (ω)ω→0 = m−1 (F ) + m−1 (F † ),

(7.24)

where m−1 is the inverse energy-weighted moment of the dynamic structure factor. In contrast to the moments with p ≥ 0, the inverse energy-weighted moments cannot be reduced in terms of commutators and they are usually evaluated through the direct calculation of the static response. Using the relation (7.12) between χ and the dynamic structure factor, as well as the antisymmetry property χ∗F (ω) = χF † (−ω), one can derive the important relation {F † , F } =

+∞ −∞

dω (SF (ω) + SF † (ω)) =

π

+∞

−∞

χF (ω) coth

βω dω, 2

(7.25)

also known as the ﬂuctuation–dissipation theorem. Equation (7.25) relates the dissipative component χ of the response function to the ﬂuctuation {F † F } of the operator F . Using the property χ (ω) coth βω ≥ χ (ω)2/βω, which holds for both positive 2 and negative ω, and the identity χF (0) =

1 π

+∞

dω −∞

χF (ω) , ω

(7.26)

94

Linear Response Function

which follows from the Kramers–Kronig relation (7.16), one derives the inequality {F † , F } ≥ 2kB T χF (0),

(7.27)

which becomes an identity in the classical regime of high temperatures where coth βω 2 = 2/βω.

7.2

Density response function

In this section we apply the formalism of linear response theory to the most important problem of the density response function (Pines and Nozi`eres, 1966). Let us consider the q-component ρq =

N

−iq·ri

e

=

dre−iq·r n(r)

(7.28)

i=1

of the density operator n(r) =

N

δ(r − ri ),

(7.29)

i=1

where ri is the coordinate operator relative to the i-th particle. We will use the notation ρq to indicate the Fourier transform of n(r) in order to avoid confusion with the notation np , used in the rest of this volume to specify the particle occupation number. The density response function, hereafter called χ(q, ω), is obtained by making the choice F = G = δρ†q , with δρ†q = ρ†q − ρ†q eq in eqn (7.3). The average < ρ†q >eq is taken at equilibrium and vanishes in uniform systems if q = 0. One can write

|m|δρ†q |n|2 1 −1 −βEm |m|δρq |n|2 − . χ(q, ω) = − Q e ω − ωnm + iη ω + ωnm + iη m,n

(7.30)

Analogously, the dynamic structure factor S(q, ω) takes the form (see eqn (7.4) with F = δρ†q )) S(q, ω) = Q−1

e−βEm |n|δρ†q |m|2 δ(ω − ωnm ).

(7.31)

m,n

The dynamic structure factor characterizes the scattering cross-section of inelastic reactions where the scattering probe transfers momentum q and energy ω to the system. Let us suppose that the probe particle is weakly coupled to the system, so that the scattering process may be described in the Born approximation and the perturbation may be written in the form Hpert = vq δρ†q e−iωt eηt + h.c. ,

(7.32)

Density response function

95

where vq is the Fourier transform of the external perturbation. Under these conditions the probability P (q, ω) per unit time that the probe transfers momentum q and energy ω to the system is related to the dynamic structure factor through the relation P (q, ω) = 2π|vq |2 S(q, ω).

(7.33)

An important example of such inelastic reactions is neutron scattering from liquid helium (see the next chapter). For low-momentum transfer the response function χ(q, ω) is sensitive to the collective oscillations of the system. These are phonons in the case of uniform Bose–Einstein condensed systems. In the high-q limit the collective features of the systems are not instead relevant since the probe scatters incoherently from the individual constituents of the system. This regime is suitable for investigating the momentum distribution n(p) of the sample, a quantity of major interest in the presence of Bose–Einstein condensation. In the high-q regime the dynamic structure factor can be written as S(q, ω) =

(p + q)2 p2 dpn(p)δ ω − + , 2m 2m

(7.34)

also known as the impulse approximation (Hohenberg and Platzman, 1966), and is uniquely determined by the momentum distribution of the sample. Inserting expression (2.9) into (7.34) one predicts a delta peak centred at the recoil frequency ωr = q 2 /2m, due to the occurrence of BEC. The situation is, however, not so simple in actual systems. For example, in the case of helium ﬁnal-state interactions cannot be neglected even for the largest available values of q and are responsible for a broadening of the peak with respect to prediction (7.34). In trapped atomic gases an additional broadening is produced by the ﬁnite size of the sample. These topics will be discussed in Chapters 8 and 12. Let us now discuss the behaviour of the moments mp (q) = p+1

+∞

ω p S(q, ω)dω

(7.35)

−∞

of the dynamic structure factor. In many cases these can be evaluated through the method of sum rules. This approach is particularly useful if the dynamic structure factor S(q, ω) exhibits a sharp peak, exhausting a signiﬁcant fraction of these moments. The derivation of sum rules is simpliﬁed by using the identity S(q, ω) = S(−q, ω),

(7.36)

which holds if the unperturbed conﬁguration is invariant with respect to either parity or time-reversal transformations. This is ensured in most of the situations discussed in this volume. An important example of violation of this invariance is provided by spin-orbit-coupled Bose–Einstein condensates (see Section 21.4).

96

Linear Response Function

Let us ﬁrst consider the p = 0 moment. Using the completeness relation n |nn| = 1 and eqn (7.36) one easily ﬁnds the result m0 (q) =

+∞

S(q, ω)dω = N S(q)

(7.37)

−∞

for the non-energy-weighted moment, where S(q) =

1 (ρq ρ−q − |ρq |2 ) N

(7.38)

is the static structure factor determined by the ﬂuctuations of the density. The average is taken on the equilibrium conﬁguration of the system which coincides with the ground state if one works at zero temperature. The static structure factor is related to the two-body density matrix ˆ † (r1 )Ψ ˆ † (r2 )Ψ(r ˆ 1 )Ψ(r ˆ 2 ) n(2) (r1 , r2 ) = Ψ

(7.39)

through the expression S(q) = 1 +

1 N

dr1 dr2 [n(2) (r1 , r2 ) − n(r1 )n(r2 )]eiq·(r1 −r2 ) .

(7.40)

In uniform systems the two-body density matrix depends only on the relative distance s = r1 − r2 and eqn (7.40) becomes S(q) = 1 + n ds[g(s) − 1]eiq·s (7.41) or, equivalently, 1 g(s) = 1 + n(2π)3

dq[S(q) − 1]e−iq·s ,

(7.42)

where n = N/V is the density and g(s) = n(2) (s)/n2 is the pair correlation function. At small q the static structure factor is sensitive to thermal and dynamical correlations. However, at high q it approaches the model-independent value S(q)q→∞ = 1. In this limit the sum ρ†q ρq = ij exp[iq · (ri − rj )] entering eqn (7.38) is exhausted by the i = j term. Equations (7.39)–(7.42) show that valuable information on two-body correlations can be inferred from the study of the dynamic structure factor. Another important sum rule is given by the energy-weighted moment m1 (q) = 2

+∞

S(q, ω)ωdω = −∞

1 [δρ†q , [H, δρq ]], 2

(7.43)

involving the double commutator between the Hamiltonian and the density operator. Result (7.43) is easily obtained using the completeness relation and the identity (7.36).

Density response function

97

The energy-weighted moment ﬁxes the high-ω behaviour of the response function, as can be seen from eqn (7.23) (the term in 1/ω identically vanishes in this case): lim χ(q, ω) =

ω→∞

2 m1 (q). (ω)2

(7.44)

For velocity-independent potentials only the kinetic energy contributes to the commutator [H, δρq ], which becomes [H, δρq ] = −q · jq ,

(7.45)

where jq =

1 [pi e−iq·ri + e−iq·ri pi ] = 2m i

dre−iq·r j(r)

(7.46)

is the q-component of the current density operator j(r) =

1 [p δ(r − ri ) + δ(r − ri )pi ]. 2m i i

(7.47)

The double commutator of (7.43) yields [ρq , [H, ρ−q ]] = N 2 q 2 /m, and one ﬁnally ﬁnds the model-independent result m1 (q) =

+∞

2

S(q, ω)ωdω = N −∞

2 q 2 , 2m

(7.48)

also known as the f -sum rule (Placzek, 1952; Nozi´eres and Pines, 1958). This sum rule, which is the analogue of the popular dipole Thomas–Reich–Kuhn sum rule for atomic spectra, is remarkable from several points of view. On one hand, it holds for a wide class of interacting many-body systems, independent of statistics and temperature. On the other hand, as we will see later, it can be usefully employed, together with other moments, to estimate the frequency of the collective excitations. The f -sum rule has a direct connection with the equation of continuity. In fact, by taking the average of the Fourier transform of eqn (7.45) on an arbitrary conﬁguration out of equilibrium, one recovers the familiar equation of continuity ∂ n(r) + ∇·j(r) = 0 . ∂t

(7.49)

Due to this connection the f -sum rule is also said to express the conservation of the particle number. Let us now discuss the inverse energy-weighted moment m−1 (q) =

+∞

−∞

1 S(q, ω)dω. ω

(7.50)

98

Linear Response Function

This moment is related to the static response through the relation (see eqn (7.24)) N χ(q) ≡ χ(q, 0) = 2m−1 (q).

(7.51)

In uniform systems the low-q limit of the static response is related to the isothermal compressibility. In fact, in this case the deformations induced by the external force can be exactly expressed in terms of the local changes of the pressure, and a simple calculation yields the result (compressibility sum rule) +∞ N 1 lim S(q, ω) dω = , (7.52) q→0 −∞ ω 2mc2T where 1/rmc2T is the isothermal compressibility of the medium. Equation (7.52) is known as the compressibility sum rule. While the m1 and m−1 moments correspond to important limits (high and low frequency limits, respectively) of the response function χ (see eqns (7.44) and (7.51), +∞ respectively), the relationship between m0 = −∞ S(q, ω)dω and χ is less immediate. The dissipation ﬂuctuation theorem (7.25), applied to the density operator, provides the important relation +∞ +∞ βω N S(q) = dω. (7.53) dωS(q, ω) = χ (q, ω) coth 2π 2 −∞ −∞ When q is small the integral (7.53) is dominated by the ‘classical’ region |ω| kT and one can replace coth βω/2 with 2kB T /ω. Using eqns (7.11) and (7.52) one then obtains the low-q behaviour of the static structure factor at ﬁnite temperature: lim S(q) =

q→0

kB T . mc2T

(7.54)

At very low T the validity of (7.54) is limited to a very small interval of wave vectors. In this case one ﬁnds important ranges of q where the integral (7.53) is not exhausted by the ‘classical’ region |ω| kT and the static structure factor is sensitive to the presence of quantum ﬂuctuations.

7.3

Current response function

A useful application of linear response theory concerns the study of the current response function. This problem is of high physical interest because of the possibility of understanding some important implications of superﬂuidity. We have already introduced the current operator in eqn (7.46). It is useful to distinguish between the longitudinal and transverse components of this operator. Let us take the vector q oriented along the z-axis. The longitudinal (L) and transverse (T ) components are given by 1 z,x −iqzi (p e + e−iqzi pz,x i ), 2m i=1 i N

jqL,T =

(7.55)

Current response function

99

and correspond, respectively, to the components of the current parallel and orthogonal to q. By setting F = G = jqL,T in the general expression (7.3) one ﬁnds the following expressions for the static (ω = 0) current response: χL,T (q, 0) =

1 2 −1 −βEm Q e |m|jqL,T |n|2 , ω nm m,n

(7.56)

where we have again used the fact that the unperturbed conﬁguration is characterized by parity or time-reversal symmetry. The formalism can be easily generalized to the tensor 2 1 χm (q, 0) = Q−1 e−βEm m|(jq ) |nn|(jq )†m |m , (7.57) ωnm m,n where (jq ),m are the and m components of the current operator jq . For isotropic systems this tensor can be written in the useful form q qm q qm χm (q, 0) = 2 χL (q, 0) + δm − 2 χT (q, 0), (7.58) q q with χL and χT given by (7.56). The evaluation of the longitudinal response is straightforward. In fact, the commutation relation (7.45) can be written as [H, δρq ] = −qjqL , and χL reduces to χL (q, 0) =

1 N [δρq , [H, δρ†q ]] = , 2 q 2 m

(7.59)

where, in the last equality, we have used the f -sum rule (7.48). Equation (7.59) shows that the static longitudinal response is model independent and ﬁxed by the total number of particles. This result is very general and holds for any value of q, for Bose as well as Fermi systems. However, the evaluation of χT cannot be carried out so easily. In fact, when q → 0, the transverse response may approach a diﬀerent value. To understand the physical origin of this behaviour it is useful to express the tensor (7.58) in terms of the ﬂuctuations of the current operator. Applying the ﬂuctuation– dissipation theorem (7.25) to the current response function one ﬁnds, for small q, the identity (jq† ) (jq )m = kB T χm (q, 0).

(7.60)

By comparing eqn (7.60) with result (6.87) derived using the theory of two-ﬂuid hydrodynamics, one obtains the important relationship lim χT (q, 0) =

q→0

ρn N . ρ m

(7.61)

Equation (7.61) permits us to identify the normal (nonsuperﬂuid) density ρn in terms of the macroscopic limit of the transverse response function. The same comparison

100

Linear Response Function

provides a consistent description of the longitudinal response function, which agrees, as expected, with result (7.59). In terms of the normal and superﬂuid density the response function (7.58), in the long-wave length limit, can be written as N q qm lim χ,m (q, 0) = . (7.62) ρ + δ ρ s m n q→0 mρ q2 It is ﬁnally worth noticing that the diﬀerence between χT and χL reﬂects the occurrence of long-range eﬀects in the current response. Let us, in fact, write the tensor (7.57) in terms of its Fourier transform: χm (q) = dsχm (s)eiq·s . (7.63) If the function χij (s) does not have a long-range tail one can safely expand (7.63) for small q and the longitudinal and transverse responses coincide, being independent of the direction of q. Another important example of transverse response is given by the static response to a rotational ﬁeld, which deﬁnes the moment of inertia. This quantity can be measured experimentally and provides a useful indicator of superﬂuidity. Its behaviour will be extensively discussed in the following chapters, in the context of both superﬂuid helium and of trapped atomic gases.

7.4

General inequalities

Using the formalism of linear response function it is possible to derive several inequalities of general validity. Some of them will be applied in other chapters of this volume to discuss speciﬁc problems of physical relevance. A ﬁrst class of inequalities can be derived at T = 0 (ground state), where the dynamic structure function has the property of vanishing for ω < 0 (see eqn (7.5) and Figure 7.2). As a consequence one can derive rigorous upper bounds for the energy ωmin of the lowest state excited by the operator F in the form ωmin ≤

mp+1 , mp

(7.64)

which holds for any value of p. Analogously, one can easily prove that the moments (7.18) satisfy the inequalities mp+1 mp ≥ . mp mp−1

(7.65)

For p = 0 eqn (7.65) can be written as m0 ≤

√ m1 m−1 ,

(7.66)

and provides an upper bound to the non-energy-weighted moment m0 . The above inequalities become identities only if a single excited state of the system exhausts the

101

S(q, ω)

General inequalities

ωmin

ω

Figure 7.2 Schematic representation of the dynamic structure factor at T = 0. The strength vanishes for negative values of ω. In the ﬁgure the dynamic structure factor consists of a sharp peak, corresponding to the excitation of a collective mode, and of a broader structure at higher frequencies.

strength of the operator F or, in other words, if the dynamic structure factor has a delta structure of the form SF (ω) ∝ δ(ω − ω). In this case ωmin = ω and the ratios mp+1 /mp coincide with ω for any value of p. The most famous application is obtained choosing the density operator ρq for F . Setting p = 0 and using results (7.37) and (7.48) one ﬁnds that a useful upper bound to ωmin is given by the so-called Feynman energy (Feynman, 1954) ωF (q) =

2 q 2 m1 (q) = , m0 (q) 2mS(q)

(7.67)

which provides a useful estimate of the energy of the elementary excitations in terms of the static structure factor. The Feynman estimate (7.67) has been extensively used to discuss the excitation spectrum of superﬂuid helium as a function of q (see Chapter 8). Alternatively, eqn (7.66) takes the form S(q) ≤

2 q 2 χ(q), 4m

(7.68)

where we have used the f -sum rule result for m1 , and m−1 has been expressed in terms of the static response function (see eqn (7.51)). This result is particularly useful at small q where χ(q) approaches the compressibility 1/mc2 with the consequence that, at T = 0, S(q) vanishes like S(q) ≤

q 2mc

(7.69)

102

Linear Response Function

as q → 0. In the same limit, using the inequality m1 ωmin ≤ , m−1

(7.70)

which also holds at T = 0, one ﬁnds that the lowest excitation frequency ωmin vanishes like ωmin (q) ≤ cq.

(7.71)

The above results have been derived on a very general basis, without any assumption as to the nature of the system, except the validity of the f -sum rule and the fact that the compressibility is ﬁnite. As emerges from eqns (7.69) and (7.71), these simple assumptions are suﬃcient to prove that the excitation spectrum is gapless and that the density ﬂuctuations, given by S(q), are vanishingly small in the long-wavelength limit. As we will see in Section 7.6, the bounds (7.69) and (7.71) become identities in the case of the weakly interacting Bose gas where all the moments are exhausted by a single excited state. Actually, in the dilute Bose gas this is true for all values of q. It is also remarkable that in superﬂuid helium, a system characterized by strong correlations, the bounds (7.69) and (7.71) become identities in the small-q limit. At ﬁnite temperatures an important inequality derivable from the formalism of response function is the so-called Bogoliubov inequality (Bogoliubov, 1962) |χF † G (0)|2 ≤ χF (0)χG (0),

(7.72)

involving the static response of two generic operators F and G and we have set χF ≡ χF † F and χG ≡ χG† G . The static response is deﬁned by the equation (see eqn (7.3) with ω = 0):

m|F † |nn|G|m m|G|nm|F † |n 1 , (7.73) χF † G (0) = Q−1 e−βEm + ωnm ωnm m,n where we have assumed, without any loss of generality, that the expectation values of F and G vanish at equilibrium. If the operators F or G do not commute with the ˆ then it is convenient to work within the grand canonical particle number operator N ensemble, replacing the energies Em with the grand canonical energies Em − μN . Inequality (7.72) is the consequence of Schwartz inequality applied to the scalar product between two operators F and G deﬁned by (F, G) ≡ χF † G (0). One can, indeed, easily verify that the quantity χF † G (0) satisﬁes all the requirements needed to apply the Schwartz inequality. In particular, linearity follows from the deﬁnition of the static response, and the condition (F, F ) ≥ 0 is guaranteed if the system is in thermodynamic equilibrium. In fact, by virtue of the relationship (7.12), the static response (7.26) is always positive. We can now combine the inequality (7.72) with the inequality (7.27): {F † , F } ≥ 2kB T χF (0),

(7.74)

General inequalities

103

following from the ﬂuctuation–dissipation relation (7.25). Furthermore, by deﬁning the operator C according to G = [H, C], one ﬁnds the useful identities χG (0) = [C † , [H, C]] and χF † G (0) = [F † , C], which simply follow from deﬁnition (7.73) and the use of the completeness relation. In terms of the operators F and C, the inequality (7.72) ﬁnally implies the result {F † , F } ≥ 2kB T

|[F † , C]|2 , [C † , [H, C]]

(7.75)

also called Bogoliubov inequality. Equation (7.75) provides a rigorous lower bound to the ﬂuctuations of a general operator F in terms of the auxiliary operator C. This inequality has been used to prove the absence of long-range order in an important class of two-dimensional and one-dimensional problems with continuous symmetry (Mermin and Wagner, 1966; Hohenberg, 1967). A useful application of the Bogoliubov inequality (7.75) is given by the study of the infrared behaviour exhibited by the particle distribution np of a Bose–Einstein condensed system. Let us make the choice F = ap , C = ρ†q with q = p/, where ap is the usual particle annihilation operator, while ρq is the density operator (7.28) which, in second quantization, takes the form ρ†q = k a†k+q ak , with the sum running over a complete set of values k = 2πn/L. With the above choices one easily ﬁnds the result {F † , F } = 2np + 1,

(7.76)

showing that the ﬂuctuation of the operator F is determined by the particle occupation number np = a†p ap , i.e. by the momentum distribution of the system (see eqn (2.17)). Furthermore, one easily ﬁnds the results [F, C] = a0 = n0 N (7.77) and [C, [H, C † ]] = N

p2 , m

(7.78)

where n0 = N0 /N is the condensate fraction and, in deriving (7.77), we have √ assumed gauge symmetry breaking, together with the Bogoliubov prescription a0 ≡ N0 . Equation (7.78) instead coincides with the f -sum rule. Collecting the above results the inequality (7.75) ﬁnally takes the form 2np + 1 ≥ m

2kB T n0 . p2

(7.79)

This inequality was used by Hohenberg (1967) to rule out BEC in two-dimensional and one-dimensional systems. It exploits the characteristic 1/p2 infrared divergency already discussed in Section 6.7. The present derivation represents a rigorous proof, based only on the validity of the f -sum rule and on the existence of the spontaneous breaking of gauge symmetry, associated with Bose–Einstein condensation. Actually,

104

Linear Response Function

result (7.79) has also been derived assuming that the system is in thermal equilibrium and turns out to be useful only at ﬁnite temperature. According to the discussion of Section 6.7 (see eqn (6.84)), one can interpret result (7.79) as the consequence of the thermal ﬂuctuations of the phase which are properly taken into account by the Bogoliubov inequality (7.75). At T = 0, where only quantum ﬂuctuations survive, the Bogoliubov inequality does not provide any useful information on the ﬂuctuations of the operator F . It is therefore interesting to look for an alternative inequality which directly exploits the eﬀects of quantum ﬂuctuations. The new inequality is provided by the uncertainty relation relative to the two operators F and C. By applying the Schwartz inequality to the scalar product deﬁned by (A, B) ≡ A† , B, one derives the inequality # # F † F C † C + F F † CC † ≥ |F † C| + |CF † | ≥ |[F † , C]|. From this inequality, noting that |a| + |b| ≥ 2 |a||b|, and choosing a = F † F CC † , b = F F † C † C, one obtains the result | [F † , C] |2 , {C † , C}

{F † , F } ≥

(7.80)

which also provides a lower bound for the ﬂuctuations of a general operator F in terms of the auxiliary operator C. It is worth comparing the uncertainty inequality (7.80) with the Bogoliubov inequality (7.75). Both provide rigorous bounds. However, in contrast to from eqn (7.75), the uncertainty inequality (7.80) does not depend explicitly on temperature and can also be used at T = 0. Let us make the same choice as before, namely F = ap and C = ρq , where q = p/. The quantity {C † , C} is proportional to the static structure factor S(q) (see eqn (7.38)) and hence, using results (7.76) and (7.77), one ﬁnally ﬁnds the nontrivial result (Pitaevskii and Stringari, 1991) 2np + 1 ≥

n0 , 2S(p/)

(7.81)

which provides a rigorous bound to the particle distribution function np in terms of the static structure factor. Equation (7.81) establishes that, in the presence of Bose– Einstein condensation, the ﬂuctuations of the phase (accounted for by np ) and the ﬂuctuations of the density (accounted for by S(p/)) cannot simultaneously be too small. This inequality has an important consequence in the small-p limit where, at T = 0, one can use the further inequality (7.68)–(7.69) for the static structure factor. One then ﬁnds that, when p → 0, the particle distribution function diverges as np ≥

n0 mc . 2p

(7.82)

This infrared divergency is the consequence of two-body interactions which make the compressibility of the system ﬁnite. The 1/p divergency in the momentum distribution of a Bose–Einstein condensed system was ﬁrst identiﬁed by Gavoret and

Response function of the ideal Bose gas

105

Nozi`eres (1964). The inequality (7.82) has important consequences in one-dimensional systems, where it permits us to rule out the occurrence of long-range order in Bose systems at T = 0 (see Section 24.3).

7.5

Response function of the ideal Bose gas

In the ideal Bose gas the density response function can be calculated analytically. This is an instructive application of the formalism developed in the previous sections, even if one should always keep in mind that this model is inadequate to describe the dynamics of the gas at small q due to the role of interactions (see next section). The matrix element m|δρq |n entering eqns (7.30) and (7.31) for χ(q, ω) and S(q, ω) is easily calculated by writing ρq in the formalism of second quantization: ρq =

p

a†p−q ap .

(7.83)

Since, in the ideal gas, the eigenstates of H are ﬁxed by the occupation numbers np of each single-particle state, the matrix element m|a†p−q ap |n vanishes unless the energy diﬀerence En − Em is equal to the diﬀerence 0 (p + q) − 0 (p) = 2 q 2 /2m + q · p/m between the single-particle energies 0 (p) = p2 /2m. Using the completeness relation n |nn| = 1 and the property np np+q = np np+q , which hold in the ideal gas, the imaginary part of the response function and the dynamic structure factor become, respectively, 2 q 2 χ (q, ω) = π − q·p (7.84) (np − np+q )δ ω − 2m m p and S(q, ω) =

p

2 q 2 − q·p , np (1 + np+q )δ ω − 2m m

(7.85)

where np = a†p ap is the average occupation numbers of particles, given by np = (exp[β(p2 /2m−μ]−1)−1 . Result (7.84) also holds for a Fermi gas, where, of course, np should be evaluated according to Fermi statistics. The dynamic structure factor of the Fermi gas is instead obtained by replacing (1 + np+q ) with (1 − np+q ) in eqn (7.85). In the presence of Bose–Einstein condensation one should separate the contribution arising from the condensate and integrate the rest of the sum. The result for χ is

2 q 2 2 q 2 + dp˜ n(p)δ ω − − q · p −[ω → −ω], χ (q, ω) = π N0 (T )δ ω − 2m 2m m (7.86) where n ˜ (p) = V /h3 np is the momentum distribution of the particles out of the condensate (see deﬁnition (2.9)). Equation (7.86) is characterized by a sharp peak at ω = ±q 2 /2m and by a continuum of excitations arising from the thermal component

106

Linear Response Function

of the gas. The delta peak represents the leading contribution at low temperature (T Tc ), where N0 (T ) ∼ N , and in this regime the function (7.86) approaches the T = 0 value

2 q 2 2 q 2 χ (q, ω) = πN δ ω − − δ ω + . (7.87) 2m 2m In the same limit the dynamic structure factor becomes

2 q 2 2 q 2 N δ ω − − δ ω + . S(q, ω) = 1 − exp[−ω/kB T ] 2m 2m

(7.88)

Unlike χ , the dynamic structure factor exhibits an important temperature dependence, despite the fact that T Tc . By integrating (7.88) one obtains the result +∞ 2 q 2 S(q) = (7.89) dωS(q, ω) = coth N −∞ 4mkB T for the static structure factor, which approaches the value 1 when q is much larger than the inverse of the thermal wavelength λT = 2π2 /mkB T . For wave vectors q 2 2 smaller than λ−1 T , eqn (7.89) instead exhibits the divergent behaviour 4mkT / q , reﬂecting the inﬁnite compressibility of the ideal gas in the presence of Bose–Einstein condensation (see Figure 7.3). 4

kBT = 4mc2

S(q)

3

2

1

0

0

1

2

3

4

5

qξ

Figure 7.3 Static structure factor as a function of the dimensionless variable qξ, calculated in an interacting Bose–Einstein condensed gas at the temperature kB T = 4mc2 . The dashed line gives the prediction of the ideal gas. Interaction eﬀects are important at low momenta. As q → 0 the static structure factor approaches a ﬁnite value as a consequence of interactions which make the compressibility of the gas ﬁnite.

Response function of the weakly interacting Bose gas

7.6

107

Response function of the weakly interacting Bose gas

In Chapter 3 we presented the Bogoliubov theory of weakly interacting gases. This theory can be applied to temperatures much smaller than the critical value (T Tc ), where the thermal depletion of the condensate is small. Furthermore, the theory is valid for values of the gas parameter satisfying the condition na3 1 of weak interactions. Using result (3.28) for Tc it is can quickly be seen that this condition is equivalent to requiring that the chemical potential μ = mc2 should also be much smaller than the critical temperature (μ kB Tc ). However, the temperature T does not necessarily have to be smaller than μ/kB . The evaluation of the matrix elements of the density operator is simpliﬁed by the fact that, as a consequence of the Bogoliubov transformation (4.23), the Hamiltonian takes the diagonalized form (4.29). The eigenstates of the Hamiltonian are consequently classiﬁed in terms of the occupation numbers of the quasi-particle excitations, the ground state corresponding to the vacuum of quasi-particles. The strategy then consists of writing the density operator (7.83) in terms of the creation and annihilation operators of quasi-particles. Within the accuracy of the Bogoliubov approach, one has √ ρq = N (a†q + a−q ), (7.90) which, using the Bogoliubov transformation (4.23), reduces to √ ρq = N (uq + vq )(b†q + b−q ),

(7.91)

where the Bogoliubov amplitudes u and v have been chosen to be real and invariant under the change of q into −q (see eqn (4.28)). After some simple algebra, one ﬁnds the result χ (q, ω) = π

2 q 2 N [δ(ω − (q)) − δ(ω + (q))] 2m(q)

(7.92)

for the imaginary part of the response function, where we have introduced the Bogoliubov energy of elementary excitations (4.31) and, consistent with the assumption of a low temperature, we have set N0 = N . The dynamic structure factor instead takes the form S(q, ω) = N

1 2 q 2 [δ(ω − (q)) − δ(ω + (q))] . 2m(q) 1 − exp[−ω/kB T ]

(7.93)

With respect to the low-temperature predictions (eqns (7.87)–(7.89)) of the ideal Bose gas, the free-particle energy is replaced by the Bogoliubov energy (4.31) and the strength of the peaks is consequently renormalized. It is immediate to verify, using the above result for S(q, ω), that the f -sum rule (7.48) is exactly satisﬁed, while the inverse energy weighted moment is given by m−1 (q) = N

2 q 2 . 2m(q)2

(7.94)

108

Linear Response Function

In contrast to the ideal Bose gas, eqn (7.94) approaches the constant value N/2mc2 when q → 0, since (q) = cq in this limit. The ﬁniteness of the compressibility in Bose gases is an important consequence of interactions, and is properly taken into account by Bogoliubov theory. The static structure factor is also easily evaluated and takes the nontrivial form S(q) =

2 q 2 (q) coth , 2m(q) 2kB T

(7.95)

which generalizes the ideal Bose gas result (7.89) and reduces to S(q) =

2 q 2 2m(q)

(7.96)

at T = 0. Notice that the static structure factor (7.96) vanishes like S(q) →

q 2mc

(7.97)

as q → 0 (see Figure 7.4). As already pointed out this behaviour is not peculiar of the dilute Bose gas, but holds in general for interacting superﬂuids. For large q one instead ﬁnds the result S(q) → 1 −

2m2 c2 . 2 q 2

(7.98)

It is useful to discuss the behaviour of (7.95) in the two opposite regimes kB T mc2 and kB T mc2 . Since μ kB Tc both regimes are compatible with the requirement T Tc needed to apply Bogoliubov theory. 1.5 kBT = mc2/4

S(q)

1

0.5

0

0

1

2

3

4

5

qξ

Figure 7.4 Static structure factor as a function of the dimensionless variable qξ, calculated in an interacting Bose–Einstein condensed gas at the temperature kB T = mc2 /4. The dashed line gives the T = 0 prediction of Bogoliubov theory. Thermal eﬀects are important at small q and are responsible for the ﬁnite value of S(q) at q = 0, as a consequence of the ﬂuctuation–dissipation theorem.

Response function of the weakly interacting Bose gas

109

i) kB T mc2 . In this case the behaviour of S(q) is similar to the one of the ideal gas, except at small q where the thermal excitation of phonons is important and the static structure factor is determined by the compressibility sum rule, approaching the value kB T /mc2 . ii) kB T mc2 . In this regime the gas behaves like it does at T = 0, except at very small q where it approaches the ‘classical’ value kB T /mc2 . Figures 7.3 and 7.4 very clearly show that, despite the temperature of the system being very small (T Tc ) and the imaginary part of the response function having reached its T = 0 value (7.92), the static structure factor exhibits an important dependence on T . A systematic experimental investigation of the static structure factor for diﬀerent values of the coupling constant has been carried out by Hung et al. (2011) in two-dimensional Bose gases, where the pair correlation function can more easily be measured. This analysis has explicitly pointed out the diﬀerent behaviour of the structure factor discussed above at small-wave vectors, depending on the value of kB T /mc2 , and has conﬁrmed in a precise way the validity of the general result eqn (7.54), which follows from the ﬂuctuation dissipation theorem and holds for systems with ﬁnite compressibility at all temperatures, independent of their dimensionality.

8 Superﬂuid 4He Before the realization of Bose–Einstein condensation in alkali gases conﬁned in magnetic traps, liquid 4 He was for many years the only available system where the phenomena of superﬂuidity and BEC could be investigated experimentally. Helium, in the liquid phase, is a dense system. The average interatomic distance is, in fact, of the order of a few ˚ Angstr¨oms, which is the typical range of interatomic forces. As a consequence, helium behaves quite diﬀerently from a dilute gas where the smallness of the gas parameter na3 is the starting point for understanding most of its physical properties. Despite the importance of short-range correlations, liquid helium, due to the light mass of the atoms, exhibits crucial ﬂuctuations of quantum nature which prevent it from becoming solid even at zero temperature. Actually, helium is the only permanent liquid available in nature and only by increasing the pressure does it undergo a liquid–solid phase transition. Below the temperature Tλ = 2.17K liquid helium becomes superﬂuid (see Figure 8.1). Fritz London (1938) ﬁrst realized that the experimental value of Tλ is close to the critical value Tc = 3.1K for the BEC transition predicted by the ideal Bose gas model at the same density, thereby suggesting the existence of a relationship between the phenomena of superﬂuidity and Bose–Einstein condensation. London’s paper was the starting point of a series of important works aimed to explore in a deeper way the fundamental connections between these two important features characterizing degenerate Bose systems. The purpose of this chapter is to summarize some key properties exhibited by superﬂuid helium which are relevant in the general context of the book and, in particular, in connection with the physics of Bose–Einstein condensed trapped gases. For more exhaustive discussions on the superﬂuid behaviour of helium many excellent textbooks are available (see, for example, Wilks, 1967).

8.1

Elementary excitations and dynamic structure factor

Let us ﬁrst discuss the dispersion relation (p) of the elementary excitations of superﬂuid 4 He. This dispersion permits us to understand many important thermodynamic and superﬂuid properties. The dispersion law is shown in Figure 8.2 for the most relevant case of zero temperature and pressure. It exhibits a typical linear slope at low momenta followed by a maximum (maxon) and a minimum (roton) at higher momenta. This form of the spectrum was ﬁrst suggested by Landau (1947) on the basis of experimental data on relevant thermodynamic quantities. In particular, the temperature dependence of entropy and speciﬁc heat permitted the estimation of the value of

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Elementary excitations and dynamic structure factor

111

40

solid He 30

20

liquid He II

λ - line

Pressure (atm)

melting

liquid He I

10 critical point evaporation 0

1.0

2.0

3.0

4.0

He gas 5.0

Temperature (˚K)

Figure 8.1 Pressure–temperature phase diagram of 4 He. The λ-line separates the normal (He I) from the superﬂuid (He II) phase of liquid helium.

30

E /kB [K]

20

10

0

0

1

2 k

3

[Å−1]

Figure 8.2 Excitation spectrum of liquid helium at saturated pressure and a low temperature. The dotted line represents the experimental data from Donnelly et al. (1981). The points with the error bars are the quantum Monte Carlo calculations of Moroni et al. (1998). The dashed line corresponds to the Feynman upper bound (8.9). Reprinted by permission from c 1981, Springer. Journal of Low Temperature Physics, 44, 471;

112

Superﬂuid 4 He

the energy gap Δ at the roton minimum, while the measurements of the superﬂuid density gave access to the value of the momentum p0 of the roton (see eqn (8.4)). The initial part of the spectrum corresponds to the phonon linear law = cp, where the sound velocity c is deﬁned by the compressibility ∂P/∂n according to c=

1 ∂P m ∂n

1/2 .

(8.1)

In the above equation m = 6.65 × 10−24 g is the mass of a 4 He atom and n = N/V is the density. The equation of state of liquid 4 He is well known experimentally and, at zero temperature, is well reproduced by the phenomenological parameterization E 1 1 1 = bn + c2 n2 + c3 n3 N 2 2 3

(8.2)

for the energy per particle. Starting from (8.2) one can easily calculate the pressure and the compressibility using the thermodynamic relation ∂ E P = n2 . (8.3) ∂n N 6

6

A and c3 = 1.86 × In eqn (8.2) the parameters b = −719K˚ A , c2 = −2.42 × 104 K˚ 9 6 ˚ 10 KA have been ﬁxed phenomenologically to reproduce the binding energy −3 (−7.14K), the density (0.0218˚ A ), and the sound velocity (238m/sec) at zero pressure. Equation (8.2) accurately reproduces the equation of state over a wide range of pressures (see Figures 8.3 and 8.4). It predicts the value P ∼ −9 atm. for the spinodal point where the velocity of sound vanishes, in good agreement with ab initio calculations of the equation of state (Boronat et al., 1994) and consistent with the data available from cavitation experiments (Caupin and Balibar 2001). A peculiarity of the excitation spectrum of 4 He is the fact that, for a ﬁxed value of p, there are no excitations below a given energy threshold. This is a crucial condition required in order to satisfy the Landau criterion for superﬂuidity (see Section 6.1). Another important feature is the appearance of the roton minimum, whose dispersion can be presented in the form (p) = Δ +

(p − p0 )2 , 2m∗

(8.4)

with the zero-pressure values Δ = 8.7 K, p0 / = 1.9 × 108 cm and m∗ = 0.14m. The Landau critical velocity (6.1) for this type of spectrum is ﬁxed by the roton minimum: vc ≈ Δ/p0 , and turns out to be ≈ 60 m/sec, a factor four times smaller than the sound velocity. It is worth noticing that, at zero pressure, the curve of the spectrum in its initial part stays above the ‘sound line’ = cp for p/ < 0.54 × 108 cm−1 (see Figure 8.5). As a consequence, the phonons in the region above this line can decay into two or more excitations, with smaller momenta giving rise to the Beliaev decay (Maris and

Elementary excitations and dynamic structure factor

113

30

P [atm.]

20

10

0

−10 0.015

0.020

0.025

ρ [å−3] Figure 8.3 Equation of state of superﬂuid helium at a low temperature. Points— experimental data; dashed line—quantum Monte Carlo results; solid line—density functional theory. From Dalfovo et al. (1995). 400

c (m/sec)

300

200

100

0

−10

0

10

20

P [atm.]

Figure 8.4 Sound velocity in superﬂuid helium at a low temperature. Points—experimental data; dashed line—quantum Monte Carlo results; solid line—density functional theory. From Dalfovo et al. (1995).

114

Superﬂuid 4 He 0.3 c0 = 238.3 m s−1

10

0.2

Energy [K]

Energy [THz]

4He 1.2K

5

0.1

0

0

0.2

0.4 0.6 Wave vector [å−1]

0.8

0

Figure 8.5 Dispersion curve of superﬂuid helium at 1.2 K compared with the sound line. For wave vectors smaller than 0.54 ˚ A the dispersion stays above the sound line and phonons exhibit Beliaev decay. By Stirling in 1991 (from Wyatt and Lauter, 1991, p. 29). Reprinted from ‘Excitations in two-dimensional and three-dimensional quantum ﬂuids’, A.F.G. Wyatt and H.J. Lauter eds. (1991) p. 29. With kind permission from Springer Science and Business Media.

Massey, 1970; Maris, 1977) discussed in Section 6.5. The decay disappears at higher momenta so that, at zero temperature, the excitations with high enough energy, and in particular the rotons, have no damping. Beliaev damping has been detected experimentally in superﬂuid 4 He. In this experiment phonons with a well-deﬁned value of energy are generated in the liquid and revealed by a detector placed at some distance form the source. In the region where Beliaev damping takes place the mean free path of phonons is of the order of 100 ˚ A, while more energetic phonons propagate up to a few millimetres. Also, above the roton region the spectrum of elementary excitations exhibits interesting features. In particular, one can prove that, if the spectral curve reaches the energy 2Δ at some point p < 2p0 , then the excitation is unstable against decay into two rotons (Pitaevskii, 1959). Experimentally, the most powerful method to investigate the energy spectrum of liquid helium is the measurement of the dynamic structure factor S (q,ω) by means of the inelastic scattering of slow neutrons. The interaction with the scattering neutrons is described by the Hamiltonian

V (r) =

2π2 an n ˆ (r), M

(8.5)

Elementary excitations and dynamic structure factor

115

where an is the neutron–atom s-wave scattering length, M is the neutron–atom reduced mass, and n ˆ (r) is the atomic density operator. Use of the Born approximation yields the following result for the scattering probability per unit time for the neutron scattered in the momentum interval dp (see eqn (7.33)) dP (q, ω) =

a2n 1 S(q, ω)dp , M2 V

(8.6)

where S(q, ω) is the dynamic structure factor of the liquid, V is the volume, q = p − p , and ω = E − E . Here p, E and p , E are, respectively, the initial and ﬁnal momenta and energies of the neutron. At T = 0 the dynamic form factor of liquid 4 He can be parameterized in the following way:

(q) + S˜ (q, ω), (8.7) S (q, ω) = Z (q) δ ω − and is characterized by a delta contribution describing the process of creation of a single excitation and by a continuous term S˜ accounting for multiexcitations and vanishing for ω < (q)/. In eqn (8.7) we have used the wave vector q instead of the momentum p = q to label the dispersion law. Actually, eqn (8.7) does not take into account Beliaev damping eﬀects which are responsible for a smoothing of the delta peak at low q. The eﬀect of Beliaev decay is, however, very small and will be ignored in the following. The ﬁrst measurement of the dynamic structure factor in superﬂuid helium was made by Palevsky et al. (1957). At present, rather systematic experimental information about S (q,ω) is now available from neutron scattering data over a wide range of values of q and ω, not only near the delta spectral curve, but also in the region of higher energies where multi-phonon processes are important (Figure 8.6). The knowledge of S (q,ω) permits us to calculate the static form factor 1 S (q) = N

∞ S (q,ω) dω,

(8.8)

−∞

which, according to (7.40), is directly related to the two-body correlation function. The static structure factor S(q) can also be measured directly by means of the diﬀuse scattering of X-rays or neutrons (Svensson et al., 1980). The measured results of S (q) are shown in Figure 8.7 at T = 1.38K and saturated vapour pressure. This quantity is characterized by a typical maximum at q ∼ 2 × 108 cm−1 reﬂecting the intrinsic tendency to solidiﬁcation exhibited by this highly correlated liquid. Notice that, according to the ﬂuctuation-dissipation theorem, the static structure factor does not vanish as q → 0, as happens at T = 0, but approaches the value S(q) → kB T /mc2T (see eqn (7.54)). In Figure 8.8 we show the pair correlation function, related to S(q) by eqn (7.42). The theoretical determination of the pair correlation function g(r) and hence of the static structure factor has been the object of many microscopic calculations at

116

Superﬂuid 4 He

(a)

(b)

600

Q = 0.4 Å–1 T = 1.35 K

1500

20 atm. Q = 1.13 Å–1 Tλ = 1.928 K

Net intensity

400 1000

T = 1.29 K 200

500

0

0 0

0.2 0.4 Energy [THz]

0.6

–0.2

0

0.2 0.4 0.6 0.8 1.0 1.2 Energy [THz]

Figure 8.6 Measured scattering intensity from superﬂuid helium at low T for two diﬀerent transferred wave vectors Q. By Glyde in 1991 (from Wyatt and Lauter, 1991, p. 3). Reprinted from ‘Excitations in two-dimensional and three-dimensional quantum ﬂuids’, A.F.G. Wyatt and H. J. Lauter eds. (1991) p. 3. With kind permission from Springer Science and Business Media.

both T = 0 and ﬁnite temperatures. In Figures 8.7 and 8.8 we show the predictions of a path integral Monte Carlo (PIMC) simulation (Ceperley, 1995) carried out at a temperature close to the experimental value. The agreement between theory and experiment is excellent. In terms of the behaviour of the static structure factor (8.8) one can provide a qualitative explanation of the roton minimum exhibited by the energy spectrum. In fact, according to (8.7), the dynamic structure factor vanishes for ω < (q) /. As a consequence, the Feynman energy (7.67) F =

m1 2 q 2 = m0 2mS (q)

(8.9)

provides a rigorous upper bound to the energy of the elementary excitations in superﬂuid helium. Result (8.9) was ﬁrst derived by Feynman (1954) using the ansatz |ΨF = ρq |Ψ0

(8.10)

for the wave function of the excited state with momentum q. Here ρq is the Fourier component of the density operator (see eqn (7.28)) and Ψ0 is the ground state manybody wave function. Using the property H|Ψ0 = E0 |Ψ0 and the commutation rules between H and ρq , we can immediately recover result (8.9) for the excitation energy F = ΨF |H|ΨF /ΨF |ΨF − E0 . A major merit of the Feynman formula is that it explicitly relates the roton minimum to the occurrence of the maximum in the static

Elementary excitations and dynamic structure factor

117

1.5

S(k)

1

0.5

0

0

1

2 k

3

4

[Å−1]

Figure 8.7 Static structure factor at 1.38 K and saturated vapour pressure. Solid line— PIMC calculation; black and white circles—neutron and X-ray scattering measurements, respectively. From Ceperley (1995). Reprinted with permission from Reviews of Modern c 1995, American Physical Society. Physics, 67, 279;

form factor. This formula can be used to provide a ﬁrst estimate of the excitation spectrum using the experimental results for S(q) at low temperatures, without any additional theoretical calculations. As we have already pointed out in Section 7.6, in a dilute gas the Feynman estimate (8.9) coincides with the exact dispersion law for all values of q, due to the absence of multiple excitations. In a dense superﬂuid the Feynman energy instead coincides with the excitation energy only in the phonon limit q → 0. Actually, at zero temperature, the static structure factor S(q) behaves like q/(2mc) and F (q) → cq as q → 0. In this case multiphonon processes give higher-order contributions to the moments m1 and m0 , and can consequently be neglected. This is directly conﬁrmed by the experimental data of S(q, ω) (see Figure 8.6a) which show that multiphonon processes are small if q is small. The quality of the Feynman approximation becomes worse and worse as q increases, and in the roton region it overestimates the experimental data by a factor of two (see Figure 8.2). In order to improve the Feynman estimate one needs many-body approaches accounting explicitly for the eﬀects of multi-pair processes. These theories are usually based on the explicit inclusion of backﬂow and higher-order correlations in the many-body wave function. In Figure 8.2 we report the calculation of the excitation spectrum based on the method of shadow wave functions

118

Superﬂuid 4 He 1.5

g(r)

1

0.5

0

2

4

6

8

r (Å)

Figure 8.8 Low-temperature pair correlation function of liquid helium at saturated vapour pressure. Solid line—PIMC calculation at 1.21 K; circles and crosses—neutron and X-ray scattering measurements, respectively, at 1.38 K. From Ceperley (1995). Reprinted with c 1995, American Physical Society. permission from Reviews of Modern Physics, 67, 279;

(Moroni et al., 1998). The agreement between theory and experiments is especially good in the roton region. In all the ab initio calculations presented in this chapter on liquid helium the semiempiric Aziz interatomic potential was used. With respect to the traditional Lenard-Jones potential, the Aziz potential provides a better description of interatomic forces at short distances, accounting for the experimental data on atom–atom scattering over a wide range of energies.

8.2

Thermodynamic properties

At suﬃciently low temperatures the thermodynamic properties of liquid 4 He can be calculated, starting from the energy spectrum (p), using the Bose distribution function −1

(p) Np = exp −1 , (8.11) kB T giving the number of thermal excitations carrying momentum p. The main contribution to the thermodynamic functions comes from the phonon (small p) and roton regions,

Thermodynamic properties

119

where one can carry out an analytic calculation. The phonon contribution to the free energy and to the normal density are given, respectively, by eqns (4.41) and (6.11). Concerning the roton contribution, one should notice that the roton gap Δ is large compared to the temperature T . Then, one has e(p)/kB T 1 and consequently the Bose distribution reduces to the classical Boltzmann expression Np = e−(p)/kB T with (p) given by (8.4). The free energy A = E − T S is then easily calculated and takes the form Ar = −T V nr , where

nr =

e−(p)/kB T

p20 (m∗ kB T ) 21/2 π 3/2 3

1/2

dp (2π)

(8.12)

3

=

e−Δ/kB T

(8.13)

is the density of rotons. Analogously, the roton contributions to the speciﬁc heat and to the normal part (6.11) become

2 3 Δ Δ + (8.14) + Crot = V nr kB T kB T 4 5

4

C/NkB

3

2

1

0

0

1

2

3

4

T [K]

Figure 8.9 Speciﬁc heat of 4 He. Solid line—experiment at saturated vapour pressure; triangles with error bars—PIMC calculations. From Ceperley (1995). Reprinted with permission c 1995, American Physical Society. from Reviews of Modern Physics, 67, 279;

120

Superﬂuid 4 He

and ρnr =

p20 nr , 3kB T

(8.15)

respectively. The roton contribution to thermodynamics is negligible at low temperatures because of the exponential factor in nr . However, due to the large statistical weight of rotons which carry high momentum, this contribution soon becomes important by increasing T . The phonon and roton contributions to the speciﬁc heat and to the normal part are comparable at about 0.8 K and 0.6 K, respectively. From the theoretical point of view the most accurate description of the thermodynamic functions of superﬂuid helium is provided by the path integral Monte Carlo (PIMC) technique (see Ceperley, 1995 for a general review). The curve of the speciﬁc heat is shown in Figure 8.9 and reveals that this many-body approach is well suited for describing the phase transition taking place at the λ-point, providing a quantitatively correct value of the critical temperature. Analogously, in Figure 8.10 we show

1.2

1

ρs /ρ

0.8

0.6

0.4

0.2

0 0

1

2

3

4

T [K]

Figure 8.10 Ratio of superﬂuid density to total density. Solid line—measured value at saturated vapour pressure; circles with error bars—PIMC calculation. From Ceperley (1995). c 1995, American Reprinted with permission from Reviews of Modern Physics, 67, 279; Physical Society.

Quantized vortices

121

the results for the superﬂuid density as a function of temperature. Also, in this case the agreement between theory and experiments is very good. Experimentally, the ﬁrst direct measurement of the normal part ρn in superﬂuid 4 He (Andronikashvili, 1946) was obtained by using a column of circular discs oscillating around the axis of a cylinder ﬁlled with superﬂuid helium. In this experiment the column dragged the normal part while the superﬂuid remained at rest. The change in the moment of inertia then permitted the extraction of the value of ρn . It is worth pointing out that this experiment was carried out in conditions of nonstationarity. In fact, the velocity of discs was higher than the critical velocity needed for creating vortices, which, however, were not produced in the experiment. Accurate results for the superﬂuid density were also obtained from second sound measurements (Peshkov, 1944, 1946). According to equation (6.56), the second sound velocity is in fact sensitive to the ratio ρs /ρn . The experimental data for the ratio ρs /ρ (Dash and Taylor, 1957) are reported in Figure 8.10. It is worth stressing that, at low temperatures, the superﬂuid fraction is equal to 1, even in a strongly correlated liquid like 4 He, revealing that at zero temperature the whole system is superﬂuid. This behaviour is quite diﬀerent from that of the condensate fraction, as we will discuss in Section 8.4.

8.3

Quantized vortices

The occurrence of quantized vortices is another spectacular consequence of superﬂuidity. The ﬁrst experimental proof in superﬂuid 4 He was obtained by Hall and Vinen (1956) who investigated the damping of second sound, propagating perpendicular to the axis of a rotating sample. The friction between the normal and superﬂuid parts of the liquid resulted in an additional damping of sound, which turns out to be proportional to the number of vortex lines and hence, according to eqn (6.95), to the angular velocity. A direct proof of the quantization of circulation (6.89) was obtained by Vinen (1961) who placed a metallic string along the axis of a rotating capillary. At suﬃciently high angular velocities, the rotation of the liquid around the string exhibits a jump associated with the presence of a single quantum of circulation. By studying the oscillations of the string one can make inferences about the appearance of the vortex. In fact, in the absence of the vortex line these oscillations are twofold degenerated, the frequency being independent of the polarization. The circulation removes the degeneracy, giving rise to a splitting between the two frequencies. This experiment has permitted the measurement of the quantum of circulation of a single vortex line (Figure 8.11). The direct visualization of vortices was achieved in the experiments by Packard and Sanders (1972). In this experiment one injects a beam of electrons inside a rotating cylinder of liquid 4 He. Vortex lines trap the electrons, which are then accelerated along the vortical line by an electric ﬁeld and are eventually imaged after escaping from the liquid. The electrons create spots on a ﬂuorescent screen and single as well as arrays of quantized vortex lines can be imaged using this technique (see Figure 8.12). Another experiment worth mentioning is that of Hess and Fairbank (1967). In this experiment one ﬁrst puts in rotation the liquid conﬁned by a rotating cylinder

122

Superﬂuid 4 He

Number of observations

15

10

5

0

0.2

0.4

0.6 0.8 1.0 Circulation in units of h/m

1.2

1.4

Figure 8.11 Histogram showing the values of the circulation in Vinen’s experiment. From Wilks (1967). Reprinted from The Properties of Liquid and Solid Helium, J. Wilks (1967), p. 234, ﬁg. 24. By permission of Oxford University Press.

above Tλ . The system is then cooled down into the superﬂuid phase, and by measuring the changes in the angular velocity of the vessel one can extract the corresponding changes in the moment of inertia of the liquid. Diﬀerent scenarios take place as a function of the angular velocity of the container. For angular velocities smaller than the critical value (see eqn (6.93)) Ωcr =

R ln mR2 rc

(8.16)

one predicts that no vortices can be created in the liquid. As a consequence, at suﬃciently low temperatures, no angular momentum is carried by the liquid since the system is fully superﬂuid. Equation (8.16) corresponds to the angular velocity at which, in the rotating frame, the vortical conﬁguration becomes energetically stable (see Section 6.8). The value of Ωcr is ﬁxed by the radius of the cylinder (about 0.09 cm in this experiment) and by the radius of the vortex core, which, in helium, is expected to be of the order of 10−8 cm. This yields the value ln(R/rc ) ∼ 15 and a critical frequency Ωcr /2π ∼ 1.2s−1 . By increasing the angular velocity above Ωcr one expects a jump in the angular momentum, associated with the creation of a vortex line. Additional vortices are created by increasing the angular velocity. In this experiment the precision was not suﬃcient to resolve the angular momentum of an individual vortex line but was enough to distinguish between the angular momentum of the actual superﬂuid ﬂow and that of a classical rotation (see Figure 8.13). The same authors have explored the response of the system as a function of temperature in a regime of low angular velocities, where one does not expect to excite vortices. In this case the system is partially superﬂuid because of thermal eﬀects and only the normal component contributes to the moment of inertia of the liquid. The results obtained for the angular momentum are consistent with the data for the superﬂuid density available from second sound measurements.

Quantized vortices

123

Figure 8.12 Photographs of vortex arrays in superﬂuid helium. From Yarmchuck and Packard (1982). Reprinted by permission from Journal of Low Temperature Physics, 46, 479; c 1982, Springer.

In both the Hess–Fairbank and Packard experiments it was crucial to rotate the vessel before cooling the system into the superﬂuid phase. Only with such a procedure will the thermal nucleation of quantized vortices be controllable. If one instead tries to rotate a cold superﬂuid the nucleation mechanism will be inhibited by the presence of a barrier generated by the superﬂuid component, and one is consequently forced to rotate the vessel at angular velocities much higher than the critical velocity (8.16). This behaviour is at the origin of interesting hysteresis phenomena.

124

Superﬂuid 4 He 20

15

L/L0

10

5

Uncertainty in zero

0

0

10

20 Ώ/Ώcr

30

40

Figure 8.13 Angular momentum of the superﬂuid versus angular velocity, measured after helium is cooled in rotation. The dot–dash line is the classical prediction of the rigid rotor. The solid line segments are the predictions of the vortex model. From Hess and Fairbank (1967). c 1967, American Physical Reprinted with permission from Physical Review Letters, 19, 216; Society.

The above experiments probe the macroscopic nature of quantized vortices, but do not provide any information on the microscopic structure, such as the density proﬁle of the vortex core. The microscopic structure of the vortex can be determined employing ab initio theories for the many-body wave function. The simplest approach is provided by the Feynman ansatz |Ψv = Πk eiϕk |ΨR ,

(8.17)

where ϕk is the azimuthal angle relative to the kth particle and ΨR is a many-body real wave function. Minimization of the energy with respect to ΨR , using a realistic two-body interaction, then provides the wave function of the vortex, in terms of which one can calculate the density proﬁle, energy etc. In Figure 8.14 we show a typical proﬁle calculated employing this variational technique. The ﬁgure shows that the size of the vortex is very small (∼ 1˚ A), conﬁrming that the healing length of this highly correlated system is a microscopic quantity. The oscillations exhibited by the density proﬁle of the vortex are the consequence of short-range correlations and have the typical

Momentum distribution and Bose–Einstein condensation

125

1.5

ρ/ρ0

1.0

0.5

0.0 0.0

2.0

4.0 r [Å]

6.0

8.0

Figure 8.14 Density proﬁle for a vortex at zero pressure and zero temperature. The points with the error bars are the Monte Carlo calculations by Chester et al. (1968). The full line is the density functional prediction by Dalfovo (1992). Reprinted with permission from Physical c 1992, American Physical Society. Review B, 46, 5482;

wavelength of the roton excitation. Both the core size and the density oscillations are well reproduced by the density functional approach. Actually, this phenomenological method has proven quite eﬃcient in describing many structural properties of nonuniform superﬂuids, such as surface proﬁles, ﬁlms, droplets, etc. (see Dalfovo et al., 1995). When applied to uniform bodies the density functional reduces to the typical form (8.2). Both the Feynman ansatz and the density functional calculation miss the eﬀects due to the ﬂuctuations of the vortex line, which are expected to give rise to a partial ﬁlling of the vortex core. The importance of such an eﬀect is still a subject of debate. Unfortunately, no direct measurement of the density proﬁle of quantized vortices is presently available in superﬂuid helium. In addition to vortex lines, quantized vortex rings can also be observed in superﬂuid helium. Rings are created around positive and negative ions of 4 He accelerated by an electric ﬁeld. The energy of this composite object (ring plus ion) is mainly due to the energy of the ring (Rayﬁeld and Reif, 1964), and by measuring the velocity of the ion one can check the energy–velocity relationship discussed in Section 5.4.

8.4

Momentum distribution and Bose–Einstein condensation

The discussion of elementary excitations and of the thermodynamic and superﬂuid properties of 4 He presented in the previous sections has not pointed out explicitly the

126

Superﬂuid 4 He

role of Bose–Einstein condensation. The physical quantity which more directly reveals the eﬀects of BEC is the momentum distribution. This quantity, which should not be confused with the distribution function (8.11) of elementary excitations, is related to the oﬀ-diagonal one-body density n(1) (s) by the relation (see eqn (2.5)) V n(p) = dsn(1) (s)eip·s/ = N0 δ(p) + n ˜ (p), (8.18) (2π)3 and can be calculated at both zero and ﬁnite temperature employing ab initio manybody techniques. In these calculations the occurrence of the delta function in the momentum distribution is deduced by analysis of the long-range behaviour of the onebody density matrix, which gives direct access to the condensate density n0 = N0 /V through the relation lim n(1) (s) = n0 .

(8.19)

s→∞

Almost all the available many-body calculations carried out at zero pressure and temperature predict a value of about 10% for the condensate fraction of liquid helium. Remarkably, this value is rather close to the ﬁrst estimate made by Penrose and Onsager (1956), based on a simple hard sphere model. The result for superﬂuid helium

0.5

J (Y )

0.4

0.3

0.2

0.1

0.0 –4

–2

0

2

4

Y [Å–1]

Figure 8.15 Scaling function J (Y ) measured at T = 0.35 K. No distinct condensate peak is observed. The line corresponds to a ﬁt based on impulse approximation broadened by the instrumental resolution and ﬁnal-state eﬀects. From Sokol (1995). Reprinted from Bose– Einstein Condensation, A. Griﬃn, D. Smoke, and S. Stringari eds. (1995), p. 69. With the acknowledgement of Cambridge University Press.

Momentum distribution and Bose–Einstein condensation

127

should be compared with the situation of a dilute gas, where, at zero temperature, most of the atoms are in the condensate and the quantum depletion is negligible to a ﬁrst approximation. Another important feature exhibited by n(p) in the presence of BEC is the occurrence of an infrared divergency at small p (see Section 6.7), which is at the origin of the peculiar s-dependence (6.72) of the oﬀ-diagonal one-body density at large distances. The explicit emergence of such a divergency in the numerical simulation is conditioned by the presence of the proper long-range correlations in the many-body wave function. The experimental determination of the momentum distribution of superﬂuid helium, and in particular of the condensate fraction, is a challenging problem. 15.0

12.5

n0 [%]

10.0

7.5

5.0

2.5

0.0

0

1

2 T [K]

3

4

Figure 8.16 Experimental value of the condensate fraction in superﬂuid helium as a function of temperature at a constant density of 0.147 g cm−3 (crosses). Also shown are the Green’s function Monte Carlo calculation of n0 at T = 0 (squares) and the path integral Monte Carlo calculations at ﬁnite temperatures (diamonds). From Sokol (1995). Reprinted from Bose– Einstein Condensation, A. Griﬃn, D. Smoke, and S. Stringari eds. (1995), p. 79. With the acknowledgement of Cambridge University Press.

128

Superﬂuid 4 He

In principle, neutron scattering experiments at high momentum transfer are well suited to exploring the behaviour of n(p). In fact, if the momentum transfer is much larger than the inverse of the average distance between particles, the atoms behave like independent particles. In these conditions the dynamic structure factor, which is the quantity measured in these experiments, approaches the impulse approximation (IA) limit (7.34). In the IA limit the dynamic structure factor can be rewritten in the useful form m SIA (q, ω) = J(Y ), (8.20) q which exhibits a useful scaling behaviour in the variable m q2 Y = ω− . (8.21) q 2m 15.0

12.5

Liquid

Inaccessible

Solid

n0 [%]

10.0

7.5

5.0

2.5

0.0 0.14

0.16

0.18 ρ [g/cc]

0.2

Figure 8.17 Experimental value of the condensate fraction in superﬂuid helium as a function of the density at 0.75 K (crosses). The Green’s function Monte Carlo (squares) and the hypernetted chain HNC/S (diamonds) theoretical predictions are also shown. From Sokol (1995). Reprinted from Bose–Einstein Condensation, A. Griﬃn, D. Smoke, and S. Stringari eds. (1995), p. 80. With the acknowledgement of Cambridge University Press.

Momentum distribution and Bose–Einstein condensation

129

The scaling function J(Y ) =

dpx dpy n(px , py , Y )

(8.22)

is often called the longitudinal momentum distribution (we assume here that the momentum transfer q is oriented along the z-axis). Results (8.20)–(8.22) show that, in principle, measuring the dynamic structure factor gives access to the momentum distribution of the system. In particular, the p = 0 singularity produced by Bose–Einstein condensation in n(p) should show up in a delta peak in J(Y ) at Y = 0. In practice, the situation is not so simple because ﬁnal-state interactions, which are not accounted for by the IA, can never be ignored and cause the broadening of the measured signal (see Figure 8.15). The ﬁnal analysis of experimental data, and in particular the determination of the condensate fraction, is consequently always based on model-dependent procedures. In Figures 8.16 and 8.17 we show the results for the temperature and pressure dependence of the condensate fraction extracted from these neutron scattering experiments. As expected, the condensate fraction diminishes with increasing T and P . In particular, for temperatures above Tλ and for high pressures, corresponding to the solid phase, the determined value of the condensate fraction is practically zero, supporting the reliability of the general procedure followed to extract its value (see Sokol, 1995).

9 Atomic Gases: Collisions and Trapping After general considerations about the metastability of ultracold atomic gases, in this chapter we provide a summary of some relevant interatomic collisional properties at low energy and a brief description of the most important trapping schemes, based on the interaction of atoms with magnetic and electromagnetic ﬁelds. Low-energy collisions allow for a fundamental understanding of the role of interactions in dilute gases and are determined by the s-wave scattering length. This is the basic interaction parameter that permits us to describe an important variety of many-body properties of dilute Bose–Einstein condensed gases as well as of superﬂuid Fermi gases. This interaction parameter also allows us to describe the formation of bound pairs of atoms in the presence of a Feshbach resonance. A special discussion is devoted to the study of collisional eﬀects in two dimensions (Section 9.3). The last part of the chapter illustrates typical schemes for magnetic (Section 9.4) and optical (Section 9.5) trapping, which are currently employed to conﬁne neutral atoms.

9.1

Metastability and the role of collisions

All interacting atomic systems, with the exception of helium, undergo a phase transition to the solid phase at low enough temperatures. This behaviour is illustrated in Figure 9.1, where we show a typical pressure–temperature phase diagram. In the ﬁgure we also draw the P (T ) line characterizing the BEC phase transition of the ideal Bose gas (see eqn 3.41). Above this line a dilute gas would be Bose–Einstein condensed. However, this conﬁguration is unstable since thermodynamic equilibrium, under these conditions of pressure and temperature, corresponds to the crystal phase.1 Notice that this scenario cannot be avoided since the gas in equilibrium with the solid is always classical and hence the P (T ) line separating the solid from the gas stays below the BEC line. At low temperatures the decay mechanism of the BEC gas phase is mainly dominated by three-body recombination events, which are responsible for the formation of molecules, eventually bringing the system into the thermodynamically stable solid phase. At ﬁrst sight this discussion rules out the possibility of reaching Bose–Einstein 1 An exception is provided by hydrogen atoms with parallel electronic spins. Such atoms exhibit a strong repulsive interaction and spin-polarized hydrogen remains a gas down to zero temperature (Hecht, 1959; Stwalley and Nosanow, 1976). As a result Bose–Einstein condensation of H atoms in a strong magnetic ﬁeld can be realized in true equilibrium (Fried et al., 1998).

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Metastability and the role of collisions

131

condensation. The BEC phase can however be ensured in conditions of metastability if some important criteria are satisﬁed: • The density of the gas should be so low that three-body collisions are rare. Actually, typical densities reached in the gaseous BEC regime correspond to 1013 −1015 atoms/cm3 . For higher densities recombination eﬀects become important. Such small values of the density imply that, in order to point out the eﬀects of quantum statistics, one should work at extremely low temperatures, of the order of microkelvins. • The gas should be kept far from any material wall, where the interaction with other atoms would favour the formation of molecules. The above conditions can be achieved by conﬁning a very dilute, cold and spinpolarized gas in a magnetic trap. This has actually been the natural route followed in the experiments aimed at realizing Bose–Einstein condensation in atomic gases, though it is now also possible to conﬁne and realize BEC gases in optical traps. It is not the intention of this book to discuss the various intermediate steps which have permitted the experimental realization of BEC in atomic gases. These include sophisticated cooling, trapping, and imaging techniques (for a recent review see, for example, Inguscio and Fallani, 2013). In this chapter we will mention only a few features of the trapping schemes employed for cold gases in the BEC regime which are relevant for the general discussion of the book. The fact that inelastic processes (and in particular three-body recombination) are suppressed by the diluteness of the gas and that the full equilibrium conﬁguration is characterized by the solid phase does not exclude the possibility for the gas to

P

BEC line

liquid solid

gas T

Figure 9.1 Typical P –T phase diagram. The BEC line lies in the region where the system, at equilibrium, is solid. The Bose–Einstein condensed phase of the gas can consequently exist only in conditions of metastability.

132

Atomic Gases: Collisions and Trapping

be in kinetic equilibrium with respect to two-body collisions. These collisions ensure thermalization, provided the corresponding relaxation times are signiﬁcantly shorter than the lifetime of the sample (typically a few seconds in the presently available conﬁgurations). Two-body collisions then play a crucial role in the realization of Bose– Einstein condensation in trapped atomic gases. Actually, the mechanism of evaporative cooling, which represents the last cooling step bringing the system into the BEC phase, would be impossible if the system were not able to thermalize suﬃciently fast. In evaporative cooling, high-energy atoms are allowed to escape from the sample via radio-frequency transitions so that the average energy of the remaining atoms is reduced. Two-body collisions redistribute the energy among the atoms such that the velocity distribution reassumes the statistical equilibrium form, but at a lower temperature. This allows the atomic sample to be cooled by many orders of magnitude. Two-body collisional processes are not just important for ensuring kinetic equilibrium. They are also at the origin of sizeable interaction eﬀects, which characterize in a unique way the behaviour of the gas in the Bose–Einstein condensed phase. Actually, interactions aﬀect many measurable quantities of high physical relevance like the equilibrium density proﬁles, the ground state energy and the collective frequencies. In a dilute and cold gas, collisions are properly accounted for by the s-wave scattering length, which represents the key interaction parameter for such systems. As already pointed out, three-body recombinations instead play a crucial role in the destabilization of the system and in particular in the loss rate of atoms. Kagan et al. (1985) pointed out that three-body recombinations should be a factor 3! = 6 less than in a thermal cloud at the same density, as a consequence of the quantum statistical correlations characterizing the wave function of the condensate. This eﬀect has been conﬁrmed by the experiment of Burt et al. (1997).

9.2

Low-energy collisions and scattering length

In this section we will recall some basic features of the theory of elastic scattering of slow particles (see, for example, Landau and Lifshitz, 1987b). Neglecting small relativistic spin-spin and spin-orbital interactions, the problem of calculating the scattering amplitude of two colliding atoms reduces to the solution of the Schr¨ odinger equation 2 − Δ + V (r) − E ψ (r) = 0 (9.1) 2m∗ for the relative motion with positive energy (E > 0). Here r = r1 − r2 and m∗ = m1 m2 /(m1 +m2 ) is the reduced mass of the two atoms. One needs to ﬁnd a solution of this equation in the asymptotic region r r0 , where r0 is the range of the potential V . In this region the solution can be written as ψ (r) = eikz + f (θ) where

k=

2m∗ E 2

eikr , r

(9.2)

(9.3)

Low-energy collisions and scattering length

133

and θ is the angle between the direction of r and the z-axis. The function f (θ) is called the scattering amplitude. In general it depends on the scattering energy E and determines the scattering cross-section according to 2

2

dσ = |f (θ)| dΩ = |f (θ)| 2π sin θdθ ,

(9.4)

with 0 < θ < π. As we will soon show, as E → 0 the scattering amplitude tends to a constant value, independent of E and θ: f (θ)E→0 = −a.

(9.5)

The quantity a is called the s-wave scattering length and plays a crucial role in the scattering processes at low energies. Its value is determined by the interatomic potential entering the Schr¨ odinger eqn (9.1). Result (9.4) is valid for the scattering of nonidentical particles, for example atoms of diﬀerent isotopes or atoms occupying diﬀerent states. For identical atoms the orbital part of the wave function must be symmetric or anti-symmetric, depending on whether the total spin of the two particles is even or odd. Accordingly, the cross-section takes the form 2

dσ = |f (θ) ± f (π − θ)| dΩ,

(9.6)

with 0 ≤ θ ≤ π/2. For fully polarized bosons the total spin is even, so one has to consider the positive sign in this equation. In contrast, for fully polarized fermions one has to consider the negative sign. This implies that as E → 0 the scattering crosssection of polarized fermions tends to zero, while the total cross-section for polarized bosons will approach the value σ = 8πa2 .

(9.7)

In order to calculate the scattering amplitude one must expand the wave function with respect to the values l of the angular momentum. This expansion takes the form ψ (r) =

∞ l=0

Pl (cos θ)

χkl (r) , kr

(9.8)

where Pl are the Legendre polynomials and the radial functions χkl (r) satisfy the equation d2 χkl l (l + 1) 2m∗ − χ + [E − V (r)] χkl = 0. kl dr 2 r2 2

(9.9)

For large distances r r0 one can neglect the interaction as well as the centrifugal term in (9.9). Then the solution of the equation takes the general form πl + δl , χkl (r) = Al sin kr − (9.10) 2

134

Atomic Gases: Collisions and Trapping

where δl (k) are the so-called phase shifts and k is given by eqn (9.3). Using the expansion of the exponent eikz = eikr cos θ in terms of the Legendre polynomials, namely eikz =

∞ 1 (2l + 1) Pl (cos θ) eikr − e−i(kr−πl) , 2ikr

(9.11)

l=0

and choosing Al = (2l + 1)il eiδl in order to cancel the factor e−ikr in the diﬀerence ψ − eikz (see eqn (9.2)), one easily obtains the result f (θ) =

∞ 1 (2l + 1) Pl (cos θ) e2iδl − 1 . 2ik

(9.12)

l=0

For identical particles only even or odd values of l contribute to the cross-section (9.6), depending on the symmetry of the two-body wave function. To calculate explicitly the phase shifts δl one must solve the Schr¨ odinger eqn (9.9). The situation is simple for the low-energy solutions satisfying the condition kr0 1.

(9.13)

Then, for distances r 1/k one can set E = 0 in eqn (9.9). As we will see, this reduced equation is suﬃcient to calculate the phase shifts and hence the scattering amplitude (9.12). Let us discuss the most important case of l = 0, where the reduced equation takes the form d2 χk0 2m∗ − V (r) χk0 = 0. dr 2 2

(9.14)

A schematic behaviour of the solutions of eqn (9.14) is shown in Figure 9.2(a,b) for positive and negative values, respectively, of the scattering length. The solution of (9.14) should be matched with the asymptotic form (9.10) in the region r0 r

1 . k

(9.15)

In fact, in this interval both eqns (9.10) and (9.14) are applicable. In the region r r0 one can neglect the interaction term in (9.14) and the solution takes the linear form χk0 = c0 (1 − κr),

(9.16)

the value of κ depending explicitly on the choice of the potential V (r). On the other hand, if kr 1 eqn (9.10) can also be expanded, yielding the same form (9.16) with c0 = eiδ0 sin δ0 and κ = −k cot δ0 .

(9.17)

This permits us to determine the relevant phase shift δ0 starting from the kindependent eqn (9.14). Notice that the matching condition (9.16) satisﬁed by the

Low-energy collisions and scattering length

135

function (9.10) can also be formulated in the form of the boundary condition (Bethe and Peierls, 1935)

1 dχk0 . (9.18) κ=− χk0 dr r = 0 As k → 0, eqn (9.17) yields the linear law δ0 = −

k κ

(9.19)

for the phase shift δ0 . A similar investigation shows that the phase shifts at higher values of l behave like δl ∝ k 2l+1 , and hence contribute to the low-k behaviour of (a) 1

0 χ −1

−2 0

0.5

1 r/r0

1.5

2

0

0.5

1 r/r0

1.5

2

(b) 3 2 χ

1 0 −1

Figure 9.2 Schematic behaviour of the solutions of eqn (9.14) for the scattering problem. The curves in (a) and (b) correspond to positive and negative values, respectively, of the scattering length.

136

Atomic Gases: Collisions and Trapping

the scattering amplitude (9.12) with higher-order terms. In conclusion, as k → 0 only the l = 0 term survives and one can identify the scattering length (9.5) through the relation a=−

δ0 1 = . k κ

Thus the wave function in the region (9.15) has 1 ψk0 = c0 − r

the form 1 . a

(9.20)

(9.21)

The above considerations can be presented in a diﬀerent form, which is useful for many applications. Rather than imposing the boundary condition (9.18), one can replace the real two-body potential V (r) with the ‘pseudopotential’ 2π2 a d Vˆps (r) = δ (r) r. ∗ m dr

(9.22)

It is, in fact, easy to check that the wave function (9.21) is a solution of the equation 2 − ∗ Δ + Vˆps (r) ψk0 (r) = 0. (9.23) 2m Indeed, Vˆps (r) ψk0 = −c0 2π2 δ (r) /m∗ and Δ(1/r) = −4πδ (r). Thus the use of the pseudopotential is exactly equivalent to imposing the boundary condition (9.18). In Chapters 4 and 5 we have shown that the value of the scattering length plays a crucial role in the physics of Bose–Einstein condensed gases, being the crucial interaction parameter of the theory. For this reason its knowledge, based on direct experimental measurements, is very important. The value of a is available using several experimental techniques. These include measurements based on bound state molecular and photoassociation spectroscopy as well as more macroscopic determinations of the elastic cross-section 8πa2 , based on the study of relaxation phenomena (for reviews see Dalibard, 1999 and Heinzen, 1999). The value of the scattering length, at low external ﬁelds, can range from very small values, as happens in spin-polarized hydrogen where a is of the order of the Bohr radius, to relatively large values in 87 Rb and 23 Na where a is of the order of a few nanometres. In some cases the scattering length is negative, as happens in the case of 7 Li or 85 Rb. Furthermore, as we will discuss later, in some cases the value of a can be tuned, proﬁting from the presence of a Feshbach resonance. This gives new possibilities for manipulating the interaction between atoms. For an exhaustive discussion about the values of the scattering lengths in alkalis, including the distinction between triplet and singlet conﬁgurations, we refer to Heinzen (1999) or to Pethick and Smith (2008). A complete updated review, reporting the measured scattering properties for most of the investigated atomic species and mixtures, can be found in Chin et al. (2010). An interesting case to discuss is when the two colliding atoms have a bound state at an energy just below the threshold of dissociation. In this case the radial wave

Low-energy collisions and scattering length

137

function of the bound state has the asymptotic form (for simplicity we assume here l = 0 and set m1 = m2 = m) ψ=A

e−r

√

m|ε|/

(9.24)

r

for r r0 , where ε < 0 is the energy of the bound state. If the condition

m |ε| r0 1

(9.25)

is satisﬁed, the wave function (9.24) solves the Sch¨rodinger eqn (9.9) in a wide interval of values of r r0 , where the potential V can be safely ignored. By repeating the same considerations made above, we ﬁnd that eqn (9.24) can be expanded in the form (9.21), yielding the identiﬁcation a = / m |ε|. One can then express the binding energy in terms of the scattering length as ε=−

2 . ma2

(9.26)

In general, if the value a is large, including the case of the weakly bound state discussed above, the energy dependence of the scattering amplitude is important even at small k. From the expression f = e2iδ0 − 1 / (2ik) for the s-wave scattering amplitude and result (9.17) for cot δ0 , we obtain the relationship f =−

1 , κ + ik

(9.27)

yielding, for κ = 0, the divergent behaviour σ = 8π/k2 for the cross-section (unitary limit). Actually, eqn (9.27) provides only the ﬁrst two terms of the expansion of f −1 in powers of (ik). In general, the next term, of order of k 2 ∼ E, may also be important, and in this case it is convenient to present the scattering amplitude in the form f =−

m1/2 β

1 , (E − ε0 ) / + ik

(9.28)

where β and 0 are parameters whose physical meaning will become clear. If the energy 0 is positive and β is large enough so that β 2 ε0 1, the amplitude has a strong resonant character at E = ε0 . Near the resonance (E 0 ) the scattering amplitude can be written as f ≈− 1/2

Γ/2 (mε0

1/2 /2 )

(E − ε0 + iΓ/2)

,

(9.29)

where the quantity Γ = 2ε0 /β 0 is the width of the resonance. In this case the relationship between the energy 0 of the resonance and the scattering length a, deﬁned

138

Atomic Gases: Collisions and Trapping

by (9.5), is not given by (9.26) but by the expression a = (Γ/20 )(m0 /2 )−1/2 (m0 /2 )−1/2 . In the opposite case β 2 |ε0 | 1, one can neglect E in (9.28) and we recover eqn (9.27) with κ = − m1/2 βε0 /, including the case (9.26) corresponding to 0 < 0. It is important to point out that the boundary constant κ can be very sensitive to the actual value of the interatomic potential, as well as to the presence of external ﬁelds. A particularly important situation is given by the occurrence of the so-called Fano–Feshbach resonance. While Feshbach’s work originated in the context of nuclear physics (Feshbach, 1958, 1962), Fano approached the problem from the background of atomic physics (Fano, 1961), reformulating and extending his earlier work (Fano, 1935). Nowadays, the term ‘Feshbach resonance’ is most widely used in the literature for the resonance phenomenon itself. A typical mechanism, giving rise to a Feshbach resonance in atomic physics, is illustrated in Figure 9.3. The lower line describes the potential felt by the scattering atoms in the absence of any coupling with the closed channel (upper line). In our case the closed channel may describe the interaction between atoms in

Energy

(a)

Atomic separation

Energy

(b)

Atomic separation

Figure 9.3 Mechanism giving rise to a Feshbach resonance. The lower line describes the scattering potential between two atoms in a given spin state. The upper curve represents the interaction potential in a diﬀerent spin state. By tuning the relative position between the two curves with an external magnetic ﬁeld one can realize resonance conﬁgurations (see text). In (a) and (b) the bound state is, respectively, just below and just above the threshold.

Low-energy collisions and scattering length

139

spin states diﬀerent from those considered in the scattering channel. If the magnetic moments of the atoms considered in the two channels are diﬀerent, the relative position between the two curves can be tuned continuously by changing the external magnetic ﬁeld. One can consequently go from a situation where a bound state is just below (Figure 9.3a) to a situation where the same bound state is just above (Figure 9.3b) the threshold. The transition between the two regimes takes place at some value of the magnetic ﬁeld, hereafter indicated by B0 . In the presence of a small coupling between the two channels, induced for example by exchange interactions, one consequently expects that the parameter κ, providing the behaviour of the scattering amplitude at low energy, will be positive if the state is bound (Figure 9.3a) and negative in the opposite case. By expanding κ = 0 around B = B0 and using eqn (9.20) one obtains the result a ∼ 1/(B − B0 ) for the scattering length near the resonance. Instead, if the bound state is signiﬁcantly far from the resonance the scattering length will take a constant value a ˜, so that the scattering length as a function of the magnetic ﬁeld can be usefully parameterized in the form a=a ˜ 1−

Δ , B − B0

(9.30)

where Δ ﬁxes the width of the resonance. Figure 9.4 shows the observation of a Feshbach resonance as reported by Inouye et al. (1998) for an optically trapped BEC of Na atoms. This early example highlights the two most striking features of a Feshbach resonance: the tunability of the scattering length and the fast loss of atoms in the resonance region. The latter can be attributed to strongly enhanced three-body recombination and molecule formation near a Feshbach resonance. So far we have mainly considered two identical particles involved in the scattering process, but the mechanism describing Feshbach resonances also works for atoms in diﬀerent internal states or even in cases of two atoms of diﬀerent species. In recent years a long series of Feshbach resonances in single species, multi-component, and multi-species have been experimentally observed. Chin et al., (2010) report on such measurements providing a complete scenario including single species and mixtures. In particular, the availability of Feshbach resonances in fermionic atoms occupying diﬀerent hyperﬁne states has paved the way to the realization of strongly interacting Fermi gases and to the investigation of the BCS–BEC crossover (see Chapter 16). Not all atoms or mixtures naturally possess convenient Feshbach resonances that can be used to tune the scattering length. Position and width of the resonance can in some cases represent an experimental limitation. Another mechanism that allows us to modify and ﬁnely tune interactions between atoms can be introduced by playing with the dimensionality of the system. A strong conﬁnement along one or two spatial directions can lead, for low enough temperatures, to the population of only the ground state of the harmonic oscillator along such directions and to a shift in the position of the Feshbach resonance by tuning the oscillator frequency of the conﬁning potential. This mechanism was ﬁrst theoretically predicted (Olshanii, 1998) and observed in quasi-one-dimensional geometry in fermionic (Moritz et al., 2005) and bosonic (Haller et al., 2010) systems.

140

Atomic Gases: Collisions and Trapping 10

Number of atoms N (× 105)

(a)

3

1

field ramp

0.3

field ramp

10 Scattering length a/ã α V 5rms/N

(b)

3

1

0.3 895

900

905 910 Magnetic field (G)

915

Figure 9.4 Observation of a magnetically tuned Feshbach resonance in an optically trapped BEC of Na atoms. The upper panel shows a strong loss of atoms near the resonance, which is due to enhanced three-body recombination. The lower panel shows the dispersive shape of the scattering length a, normalized to the background value a ˜ near the resonance. The magnetic ﬁeld is given in G, where 1G = 10−4 T . From Inouye et al. (1998). Reprinted by c 1998, Macmillan Publishers Ltd. permission from Nature, 392, 151;

In the case of mixtures of diﬀerent atomic species, species-selective optical manipulation (LeBlanc et al., 2007) (see Section 9.4) has led to the realization of systems with components in diﬀerent dimensionalities whose interaction is described by mixed-dimensional resonances (Massignan et al., 2006; Nishida et al., 2008; Lamporesi et al., 2010).

Low-energy collisions in two dimensions

9.3

141

Low-energy collisions in two dimensions

Modern experimental techniques permit the creation of external ﬁelds which freeze the atomic motion along the z-direction. In this case the scattering of slow atoms has a two-dimensional nature and behaves very diﬀerently with respect to the threedimensional case. We will present here a brief discussion of the corresponding theory, which holds under the condition kr0 1,

(9.31)

# where k = kx2 + ky2 is the two-dimensional wave vector of the relative motion and r0 is the range of the two-body potential. The scattering problem requires the solution of eqn (9.1), where Δ is the two-dimensional Laplacian operator and r ≡ ρ is the radius vector in the x–y plane. The asymptotic behaviour of the wave function, for ρ 1/k, can be written as eikρ ψ (ρ) = eikx + f2D √ . −iρ

(9.32)

The function f2D (k, ϕ) has the meaning of a two-dimensional scattering amplitude, ϕ being the angle between k and the x-axis. Notice that in three dimensions the analogous asymptotic equation (9.2) is valid at the weaker condition r r0 . The fac√ tor −i in the denominator is introduced to simplify the formalism. In analogy with the three-dimensional eqn (9.8), one can present the wave function as ∞

ψ=

Ql (ρ) eilϕ ,

(9.33)

m = −∞

and the low-energy scattering is dominated by the l = 0 term. As a result the scattering amplitude f2D does not depend on the angle but, in contrast to the three-dimensional case, depends on energy, as we will discuss. To ﬁnd the limiting equation for f2D satisfying the condition (9.31), let us consider the wave function on distances ρ r0 . Taking into account the isotropy of the√lowenergy scattering solution, it is suﬃcient to replace in (9.32) the function eikρ / −iρ with the exact l = 0 solution of the two-dimensional equation of the free motion 1 d dΦ r + k 2 Φ = 0, r dr dr

(9.34)

√ satisfying the asymptotic behaviour eikρ / −iρ for large ρ. The wave function satisfying this condition is ψ (ρ) = e

ikx

+ f2D

πk (1) iH0 (kρ), 2

(9.35)

142

Atomic Gases: Collisions and Trapping (1)

where H0 (x) is the Hankel function and f2D is independent of ϕ. Using the small-x expansion (1)

H0 (x)x→0 = −i

2i 2 ln , π eγ x

(9.36)

where γ is the Euler constant, we can present the wave function in the interval r0 ρ 1/k as ψ ≈ c1 − c2 ln (kr), where c1 = 1 + f2D

2k 2i ln γ , c2 = f2D π e

2k . π

(9.37)

The ratio c1 /c2 is ﬁxed by solution of the two-dimensional Schr¨ odinger equation with E = 0, in analogy to the three-dimensional case (see eqn (9.14)). Let us set c1 /c2 = ln (ka2D ), where a2D is a positive constant of dimensionality of length, which is called the two-dimensional scattering length. It is deﬁned in such a way that, for a scattering on a two-dimensional barrier of inﬁnite height, the length a2D is equal to the radius of the barrier. Then the two-dimensional scattering amplitude takes the form π 1 , f2D (k) = − 2k ln [2/ (eγ ka2D )] + iπ/2

(9.38)

and the corresponding total two-dimensional cross-section reads 2

σ2D = 2π |f2D | =

π2 1 . k ln2 [2/ (eγ ka2D )] + π 2 /4

(9.39)

For ka2D = 2e−γ the cross-section takes its maximum value 4/k. This is called the two-dimensional unitarity limit. However, due to the logarithmic dependence of the denominator, the resonance is very smooth as a function of the energy. It is well known that, if the two-body potential gives rise to a bound state with energy < 0, the scattering amplitude as a function k has a pole at the imaginary value k = i 2m∗ ||, where m∗ = m1 m2 /(m1 + m2 ) is the reduced mass of the two interacting particles. From (9.38) it follows that this divergent behaviour corresponds to the following expression for the binding energy: =−

22 m∗ (eγ a2D )

2

,

(9.40)

the size of the corresponding bound state being eγ a2D /2. The logarithmic dependence of the two-dimensional scattering amplitude is responsible for a novel behaviour of the interaction coupling constant to be used in the many-body description of dilute two dimensional quantum gases. This problem will be discussed in Chapter 23.

Zeeman eﬀect and magnetic trapping

9.4

143

Zeeman eﬀect and magnetic trapping

Magnetic trapping for neutral atoms is based on the use of inhomogeneous magnetic ﬁelds. To understand this mechanism of trapping, it is crucial to brieﬂy summarize the spin properties which determine the interaction of atomic systems with an external magnetic ﬁeld. Let us focus, for simplicity, on the case of alkali atoms (spin S = 1/2). The electronic structure of the alkalis is very simple since all the electrons, exception made for the external valence electron, occupy closed shells. As the orbital angular momentum L is zero in the ground state, the total electronic angular momentum J is equal to 1/2. The value of the nuclear spin I, instead, depends on the isotopic species. Since in the alkalis the number of protons is odd, the quantum statistical nature of the system is determined by the number of neutrons. If this number is even, then the nuclear spin is odd and the atom is a boson. On the other hand, if the number of neutrons is odd then the nuclear spin is even and the atom is a fermion. The same classiﬁcation holds for the hydrogen atom and its isotopes. The coupling between the electron and nuclear spins yields two possibilities for the total angular momentum F=I + J

(9.41)

of the atom: one has either F = I − 1/2 or F = I + 1/2. In Table 9.1 we report the quantum numbers F in the ground state of the alkali atoms. In the absence of an external magnetic ﬁeld the coupling between the electron and nuclear spins (hyperﬁne coupling) can remove the degeneracy of the two conﬁgurations. This interaction is usually represented in the form Hhf = AI·J, where A is the relevant coupling constant. One can easily express Hhf in terms of the quantum numbers I, J, and F using the standard relation I·J=

1 (F (F + 1) − I(I + 1) − J(J + 1)). 2

(9.42)

The energy splitting produced by the Hamiltonian Hhf between the two hyperﬁne states F = I ± 1/2 is then easily calculated and is given by the formula ΔE = A(I + 1/2). Typical values range between 1 and 10 GHz. In the presence of an external magnetic ﬁeld we have to add the magnetic interaction with the external ﬁeld to the hyperﬁne interaction. This yields the total Hamiltonian H = AI · J + 2μB Jz B,

(9.43)

Table 9.1 Quantum numbers in the ground state of alkali atoms.

atom

6

Li

7

Li

23

Na

39

K

40

K

41

K

85

Rb

87

Rb

133

Cs

I

1

3 2

3 2

3 2

4

3 2

5 2

3 2

7 2

F

1 3 ; 2 2

1;2

1;2

1;2

7 9 ; 2 2

1;2

2;3

1;2

3;4

144

Atomic Gases: Collisions and Trapping

where μB = |e|/2me is the Bohr magneton and z indicates the direction of the magnetic ﬁeld. In eqn (9.43) we have neglected the small contribution due to the interaction between the nuclear magnetic moment and the magnetic ﬁeld. Since the unperturbed states are eigenstates of J2 , I2 , F2 and Fz , for small magnetic ﬁelds we obtain the following result for the interaction energy between the atom and the external ﬁeld: EB = F, mF |2μB Jz B|F, mF = gF μB mF B,

(9.44)

where mF is the eigenvalue of Fz and gF =

F (F + 1) + J(J + 1) − I(I + 1) gJ 2F (F + 1)

(9.45)

is the hyperﬁne Land´e factor, with gJ being the ﬁne-structure Land´e factor (gJ 2 when L = 0 and S = J = 1/2) (Foot, 2005). For arbitrary magnetic ﬁelds the eigenstates and eigenvalues of (9.43) should be determined by diagonalization. The eigenstates will be labelled with the quantum numbers F and mF . By expressing I · J in terms of the usual raising and lowering operators according to I · J = Iz Jz + (I+ J− + I− J+ ) /2, one can easily construct the matrix elements of (9.43) on the basis |mI , mJ , with −I ≤ mI ≤ + I and mJ = ±1/2. The diagonalization of the matrix is straightforward. Let us consider the relevant case I = 3/2. The states with F = 2 and mF = ±2 are simply given by | ± 3/2, ±1/2 and one immediately ﬁnds that the energy of these states is given by 1 3 EmF = +2 = A + C 4 2

(9.46)

1 3 A − C, 4 2

(9.47)

and EmF =−2 =

where C = 2μB B. To calculate the energies of the other states we need only diagonalize 2 × 2 matrices. Let us ﬁrst consider the matrix with mJ + mI = 1. The basis of this matrix is given by |+3/2, −1/2 and |+1/2, +1/2 and the corresponding eigenvalues are 1 3 2 1 EmF =+1 = − A ± A + (A + C)2 . (9.48) 4 4 4 The eigenvalues of the matrix with mJ + mI = −1 are simply obtained by replacing C by −C: 3 2 1 1 A + (A − C)2 . EmF =−1 = − A ± (9.49) 4 4 4 Finally, the basis of the matrix with mJ + mI = 0 is given by |+1/2, −1/2 and |−1/2, +1/2. Its diagonalization yields the eigenvalues 1 1 EmF =0 = − A ± A2 + C 2 . (9.50) 4 4

Zeeman eﬀect and magnetic trapping

145

4

E/A

2

0

−2

−4

0

1

2

3

4

5

C

Figure 9.5 Hyperﬁne structure for an alkali atom with I = 3/2 as a function of the intensity of the magnetic ﬁeld.

In Figure 9.5 we plot the eight eigenvalues of the Hamiltonian (9.43). In the absence of a magnetic ﬁeld (C = 2μB B = 0) the eight levels are grouped into the two hyperﬁne levels F = 2 and F = 1 with energies E = (3/4)A and −(5/4)A, respectively. However, in the limit of high magnetic ﬁelds they approach the two levels E = ±μB B. It is also worth mentioning that the interaction between atoms occupying diﬀerent magnetic states is, in general, diﬀerent. The value of the scattering length is actually sensitive to the details of the interatomic force as well as to the value of the external magnetic ﬁeld. The rich structure of the atomic levels exhibited by alkalis and the availability of magnetic traps open important possibilities for atomic manipulation. Among them it is worth recalling the following: • The possibility of trapping atoms in diﬀerent magnetic states, allowing for the realization of mixtures of condensates of diﬀerent species trapped simultaneously in the same magnetic trap. • The possibility of inducing transitions between trapped and untrapped states (see following discussion), thereby controlling the mechanism of evaporation as well as the mechanism of coherent emission of atoms from the condensate. We are now ready to discuss the mechanism of trapping produced by a spatially varying magnetic ﬁeld. We will make the adiabatic approximation in which we assume that the variation of the direction of the magnetic ﬁeld, as seen in the atom frame, occurs on a time-scale much larger than the inverse of the Larmor frequency. This ensures that the atom will remain in the same quantum state relative to the instantaneous direction of the magnetic ﬁeld. As a consequence, if the energy of a given quantum state increases with the magnetic ﬁeld, then the atom in such a state will be driven towards the regions of low magnetic ﬁeld (low-ﬁeld-seeking states). On the

146

Atomic Gases: Collisions and Trapping

other hand, if the energy decreases with increasing magnetic ﬁeld, then the atom will be driven towards the regions of high magnetic ﬁeld (high-ﬁeld-seeking states). From result (9.44), which provides the interaction energy with the magnetic ﬁeld in the linear limit, one concludes that the low-ﬁeld-seeking states are the states in which mF = +2 and mF = +1 in the F = 2 multiplet, where the hyperﬁne Land´e factor gF (9.45) is positive, and the state mF = −1 in the F = 1 multiplet, where gF is negative. In the ﬁrst experiments on rubidium and sodium the states F = 2, mF = +2 and F = 1, mF = −1, respectively, were employed to trap the gas. It is interesting to notice that the Land´e factors (9.45) relative to the two hyperﬁne levels F = 2 and F = 1 are equal in modulus, but have opposite sign. This implies that the states F = 2, mF = +1 and F = 1, mF = −1 have the same magnetic moment (see eqn (9.44)) and consequently atoms occupying these states will feel the same conﬁning potential. It is easy to show that the modulus of a static magnetic ﬁeld cannot have a maximum in vacuum (Wing, 1984). In fact, from the relation ∇2 Bi = 0, which follows from the Maxwell equations, one derives the inequality 2 ∂Bi ∂ ∂Bi 2 2 2 ∇ B =2 Bi = 2Bi ∇ Bi + 2 > 0. (9.51) ∂xk ∂xk ∂xk This general result is incompatible with the existence of a maximum, which would require ∂B 2 /∂xk = 0 and ∂ 2 B 2 /∂x2k < 0 for each k. This proves that high-ﬁeldseeking states cannot be magnetically trapped, unless using RF of microwave dressing (Hoﬀerberth et al., 2006). Good candidates for magnetic trapping in the case of the alkalis are hence the states F = 2, mF = +2, +1 and F = 1, mF = −1. In principle, the F = 2, mF = 0 state is also a low-ﬁeld-seeker due to second-order eﬀects in the magnetic ﬁeld. Let us consider the simplest case of a linear quadrupole trap. This was the ﬁrst trap used to reach the BEC regime in alkalis. This trap is characterized by a magnetic ﬁeld which varies linearly in all directions and can be generated by two coils in an ‘anti-Helmholtz’ conﬁguration. The magnetic ﬁeld is given by the simple law B = B (x, y, −2z),

(9.52)

satisfying the conditions ∇ · B = 0 and curl B = 0. The intensity of the magnetic ﬁeld has a minimum at the origin, so that atoms occupying low-ﬁeld-seeking states will be driven towards the centre, while atoms occupying high-ﬁeld-seeking states will be driven out of the trap. Since magnetic traps only conﬁne low-ﬁeld-seeking states, atoms will be lost if they make a transition into a high-ﬁeld-seeking state. This happens if the value of the magnetic ﬁeld is so small that atoms, due to their motion, are no longer able to follow adiabatically the direction of the magnetic ﬁeld. These spin transitions are called ‘Majorana’ transitions (Majorana, 1932). In a quadrupole trap atoms spend most of the time near the centre of the trap, where the magnetic ﬁeld vanishes, and have dramatic consequences at low temperatures, where the size of the gas is small. The ﬁnal result is that quadrupole traps are not eﬃcient at hosting a BEC gas unless additional precautions are taken. The ﬁrst experimental realization of a BEC, carried

Zeeman eﬀect and magnetic trapping

147

out in Boulder, was actually achieved by superimposing a rapidly rotating, uniform magnetic ﬁeld onto the quadrupole trap (Anderson et al., 1995). The corresponding trap is known as the TOP trap. The magnetic ﬁeld in the TOP trap takes the form B = (B x + B0 cos ωt, B y + B0 sin ωt, −2B z),

(9.53)

where B is the radial gradient of the quadrupole trap, B0 is the modulus of the rotating bias ﬁeld, and ω is its angular velocity. The angular velocity should be much larger than the typical frequencies of the atomic motion so that one is permitted to take the time average for the modulus of B, but at the same time it should be smaller than the Larmor frequency so that the projection of the atomic magnetic moment on the instantaneous direction of B is constant. Typical values of ω are a few kHz. By expanding the modulus of (9.53) at short distances and taking the corresponding time ¯ one ﬁnds the result average B, 2 ¯ B0 + (B ) x2 + y 2 + 8z 2 , B 4B0

(9.54)

which explicitly shows that the magnetic ﬁeld no longer vanishes in the centre of the trap and that the resulting potential felt by atoms, given by gF μB mF B (see eqn (9.44)), is harmonic. An alternative procedure to avoid Majorana spin–ﬂip transitions was used in the ﬁrst experiment on sodium, carried out at MIT (Davis et al., 1995). In this case a tightly focused blue-detuned laser beam was added to repel the atoms from the centre of the quadrupole trap. The mechanism of interaction of atoms with the laser ﬁeld will be discussed in the next section. It is now possible to build diﬀerent types of magnetic traps, which generate harmonic potentials with the help of a static bias ﬁeld suppressing the Majorana transitions, and consequently overcome the diﬃculties of the quadrupole trap. With such traps it is possible to produce eﬀective potentials of diﬀerent symmetries, including cigar shape, triaxial, and even almost spherical traps. One of the most famous traps of this type is the so-called Ioﬀe–Pritchard trap. This trap consists of three sets of coils. A ﬁrst set is provided by two pairs of linear bars parallel to the z−axis and placed at equal distance from it. The resulting magnetic ﬁeld near the axis does not depend on z and can be described as Bx = B x,

By = −B y,

(9.55)

provided that the bars cross the x- and y-axes and the currents in adjacent bars ﬂow in opposite directions. This ﬁeld ensures the radial conﬁnement of atoms. To reach the conﬁnement in the z-direction an auxiliary set of so-called pinch coils has to be added. These coils are assumed to be coaxial and are placed at the same distance from the origin. They have the same radius and carry the same current. The magnetic ﬁeld generated by these coils near the origin is given by Bz = B0 + (B /2)(z 2 − r2 /2) and Br = −(zr/2)B , where z and r are the cylindrical coordinates. The third pair of coils, the bias coils, have a larger radius compared to the pinch coils and create

148

Atomic Gases: Collisions and Trapping

a practically uniform ﬁeld that permits the changing of the constant component B0 without disturbing the quadratic terms. By assuming that the bias ﬁeld B0 is positive and suﬃciently large, one can calculate B = |B| up to quadratic terms in z and r. The result is 1 2 1 B 2 B B = B0 + B z + r2 . − (9.56) 2 2 B0 2 The shape of the trap can then be conveniently controlled by changing the value of the bias ﬁeld B0 . All the magnetic traps mentioned here are commonly realized in the labs using coils tens of centimetres in size, placed outside the vacuum system. With the goal of miniaturization and towards the realization of transportable, atom-based devices, in the early 2000s (H¨ansel et al., 2001) the ﬁrst BEC on a chip was experimentally realized. The ﬁrst microtraps produced a very strong harmonic conﬁnement in the kHz range, with the possibility of approaching the quasi-one-dimensional regime.

9.5

Interaction with the radiation ﬁeld and optical traps

The interaction of atoms with the laser ﬁeld plays a crucial role in the manipulation of Bose–Einstein condensates and provides a rich variety of new possibilities for the conﬁnement of atomic gases, enriching the performances already available with magnetic trapping (for a general review see, for example, Grimm et al. (2000)). This interaction can be treated with high accuracy in the dipole approximation, since the wavelength of the laser radiation is much larger than the typical atomic size. In the dipole approximation the interaction can be written as V (r, t) = −d · E(r, t),

(9.57)

where d is the electric dipole operator for a single atom and E(r, t) = E(r)e−iωt + c.c.

(9.58)

is a time-dependent electric ﬁeld oscillating with frequency ω. The interaction (9.57) induces a dipole polarization in the electronic structure of the atom, which oscillates with the same frequency of the radiation ﬁeld as d = α(ω) E(r)e−iωt + c.c. ,

(9.59)

where α(ω) = −1

n

|n|d · ˆ|0|2

2ωn0 2 − (ω + iη)2 ωn0

(9.60)

is the dipole dynamic polarizability and ˆ is the unit vector in the direction of the electric ﬁeld. The polarization produces a change in the energy of the system (Stark

Interaction with the radiation ﬁeld and optical traps

149

shift), which can be calculated by using second-order perturbation theory. This energy change can be regarded as an eﬀective potential 1 U (r) = − α(ω)E2 (r, t), 2

(9.61)

felt by each atom where the bar indicates a time average. The time averaging of the potential is justiﬁed by the fact that the time variation of the laser ﬁeld (9.58) is much faster than the typical frequencies of the atomic motion. In deriving (9.61) we have assumed the applicability of linear response theory and the fact that α(ω) is a real quantity. This means that ω should not be too close to the atomic resonances where absorption processes become important. The study of absorption eﬀects requires the explicit inclusion of the imaginary part of α. In contrast to the case of the magnetic interaction energy (9.44), which is linear in B due to the intrinsic magnetic moment of the atom, the electric interaction energy (9.61) is quadratic in E as a result of the dipole atomic polarizability. Let us also recall that one should not confuse the linear response function (9.60), which concerns the electronic degrees of freedom of a single atom, with the response function introduced in Chapter 7, which instead concerns the atomic degrees of freedom of the system. If the intensity of the radiation ﬁeld varies with position, then the energy change (9.61) gives rise to a force f = α(ω)∇

E 2 (r, t) , 2

(9.62)

which aﬀects the motion of atoms. The behaviour of the force depends in a crucial way on the spatial distribution of the radiation intensity E2 (r, t) and on the exact value of the laser frequency. To appreciate the latter eﬀect let us suppose that the dipole polarizability (9.60) is dominated by a single resonant frequency ωR . In this case, the value of α depends in a crucial way on the value of the so-called detuning δ = ω − ωR , given by the diﬀerence between the laser and the resonant frequencies, and near the resonance, where |δ| ωR , the polarizability behaves like α(ω) = |R|d · ˆ |0|2 /(ωR − ω), where |R is the resonance state. The detuning should be small in order to emphasize the eﬀect of the dipole force, but should not be too small, otherwise absorption processes become important. The sign of the detuning is of crucial importance. In fact, if δ > 0 (blue detuning) the energy change (9.61) is positive and the laser ﬁeld will force the atoms to move towards regions of low ﬁeld (repulsive eﬀect). On the other hand, if the detuning is negative (red detuning) atoms will be attracted towards the regions of higher electric ﬁeld. We have already mentioned in the previous section that the interaction with a radiation ﬁeld characterized by blue detuning was used in the ﬁrst experiment at MIT to repel atoms from the centre of the quadrupole trap. In later experiments red detuning was instead employed to provide an optical conﬁnement of Bose–Einstein condensates (optical traps). Optical traps provide useful alternatives to magnetic trapping (Stamper-Kurn et al., 1998a). They can in general be tighter and leave more freedom in the choice

150

Atomic Gases: Collisions and Trapping

of the trapping frequencies along diﬀerent directions. This has led to the possibility of realizing low-dimensional systems and accessing experimentally new, interesting phenomena Actually, BEC can be achieved in optical traps without using magnetic trapping (Barrett et al., 2001). Optical traps have many advantages. Trapping is not limited to speciﬁc magnetic states and can consequently be employed to investigate the coexistence of multi-spin components (including strong-ﬁeld-seeking states) with the possible occurrence of new magnetic phases. Another interesting opportunity is given by the possibility of tuning the value of the scattering length by adding a magnetic ﬁeld. Under special conditions the interaction between atoms can become extremely sensitive to the value of the applied magnetic ﬁeld due to the occurrence of the Feshbach resonances, as discussed in Section 9.2. These modulations have been successfully implemented with the help of optical traps. The interaction with the laser ﬁeld allows for many other manipulations of Bose–Einstein condensates. For example, they can be used to build box traps, low-dimensional traps, atom guides, optical lattices, rotating traps, etc. As an illustrative example we show how the dipole force generated by the radiation ﬁeld can be used to generate an optical lattice. If the radiation ﬁeld is retro-reﬂected along the z-direction to give rise to a standing wave of the form E(r, t) = E cos(qz)e−iωt + c.c.,

(9.63)

then the time-averaged eﬀective ﬁeld (9.61) takes the form U (r) = −α(ω)E 2 cos2 (qz),

(9.64)

corresponding to a periodic potential along the z-direction with wavelength 2λ, where λ = 2π/q is the wavelength of the laser ﬁeld. This periodic potential, superimposed onto a magnetic trap, can produce an array of condensates, provided that its intensity is suﬃciently high. It is now possible to produce one-dimensional as well as two- and three-dimensional optical lattices. This permits investigation into new conﬁgurations of high physical interest. Other interesting applications of the interaction with the laser ﬁeld can be achieved using a combination of two slightly detuned laser ﬁelds. In this case, one produces a time-dependent potential whose frequency is ﬁxed by the detuning between the two lasers. The resulting time-dependent potential can be used to generate dynamic excitations in the gas, and hence to study the dynamic response of the system (see Section 12.9).

Part II

10 The Ideal Bose Gas in the Harmonic Trap The experimental realization of BEC has been achieved in atomic gases where the shape of the trapping potential is, in many cases, well approximated by a harmonic shape. For this reason it is important to understand the features exhibited by Bose– Einstein condensation in the presence of harmonic conﬁnement. In this chapter we will discuss the behaviour of the ideal Bose gas, while in the following chapters we will discuss the role of the two-body interaction by applying the general theory of nonuniform gases developed in Chapter 5. The harmonic potential model is particularly interesting because it allows for an almost analytic derivation of the relevant thermodynamic quantities. It represents a very insightful application of quantum statistical mechanics.

10.1

Condensate fraction and critical temperature

In Section 3.1 we have developed the general formalism of the ideal Bose gas in the framework of the grand canonical ensemble. This yields the result ni =

1 eβ(i −μ) − 1

(10.1)

for the average particle occupation number of the ith single-particle state, where μ is the chemical potential ﬁxed by the normalization i ni = N . In the following we will mainly be interested in the study of a gas of bosons trapped by a potential of harmonic type Vext (r) =

1 1 1 mωx2 x2 + mωy2 y 2 + mωz2 z 2 , 2 2 2

(10.2)

where ωx , ωy , and ωz are the oscillator frequencies in the three directions. Using the conﬁnement potential (10.2) the eigenvalues of the single-particle Hamiltonian H sp =

p2 + Vext (r) 2m

are given by the analytic expression 1 1 1 nx ny nz = nx + ωx + ny + ωy + nz + ωz , 2 2 2

(10.3)

(10.4)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

154

The Ideal Bose Gas in the Harmonic Trap

where nx , ny , nz = 0, 1, . . . are the quantum numbers characterizing the solutions of the corresponding Schr¨ odinger equation. The ground state of a system of N noninteracting bosons conﬁned by the potential (10.2) is obtained by putting all the particles in the lowest single-particle state (nx = ny = nz = 0) with energy 0 = (ωx + ωy + ωz )/2. The wave function of this single-particle state is given by ϕ0 (r) =

mω

ho

π

3/4

m exp − (ωx x2 + ωy y 2 + ωz z 2 ) , 2

(10.5)

where we have introduced the geometrical average ωho = (ωx ωy ωz )1/3

(10.6)

of the oscillator frequencies. The wave function (10.5) satisﬁes the normalization condition dr|ϕ0 |2 = 1. The density distribution of the N -body system becomes n(r) = N |ϕ0 (r)|2 , and grows with N . The size of the condensate is instead independent of N and is ﬁxed by the harmonic oscillator length aho =

mωho

1/2 ,

(10.7)

which corresponds to the geometrical average of the widths of the Gaussian (10.5) in the three directions. At a ﬁnite temperature some of the particles occupy the lowest state, the others being distributed among the excited states at higher energies, according to the Bose distribution function (10.1). When the number of particles in the trap is large and the temperature is signiﬁcantly higher than the ‘oscillator temperature’ ωk /kB ﬁxed by the separation between the oscillator levels, it is useful to distinguish between the particles occupying the lowest-energy state ϕ0 (condensate) and the particles occupying the higher-energy states ϕi (thermal component). According to the general criteria illustrated in Chapter 3, Bose–Einstein condensation takes place when the value of the chemical potential μ is so close to the lowest energy 0 that the occupation number N0 ≡ n0 of the i = 0 state becomes large and comparable to N . At the same time the number NT of particles of the thermal component NT =

nx ny nz =0

1 exp[β(i − μ)] − 1

can be calculated by setting μ = 0 and replacing the sum with an integral: 1 . NT = dnx dny dnz exp[β(nx ωx + ny ωy + nz ωz )] − 1

(10.8)

(10.9)

Result (10.9) is meaningful only if the value of the integral is smaller than the total number of particles. The condition for the occurrence of BEC is then ﬁxed by the inequality NT ≤ N . This condition is always guaranteed if T is suﬃciently small. The equality NT = N deﬁnes the critical temperature for Bose–Einstein

Condensate fraction and critical temperature

155

condensation, which turns out to be given by the expression (de Groot et al., 1950; Bagnato et al., 1987) kB Tc0 = ωho

N ζ(3)

1/3 = 0.94ωho N 1/3 ,

(10.10)

where ζ(n) is the Rieman function. The value of ζ(n) is reported in Table 10.1 for some choices of n frequently employed in this volume. The Rieman function coincides with the z = 1 value of the Bose function (3.26): ζ(n) = gn (1). Above Tc the chemical potential can no longer be set equal to 0 without violating the normalization condition. In this case the lowest-energy state i = 0 is occupied in a microscopic way and its contribution to the thermodynamic properties of the system becomes negligible. The temperature dependence of the condensate fraction N0 /N is easily calculated using result (10.9) and the normalization condition N0 + NT = N . One ﬁnds 3 N0 T =1− . (10.11) N Tc0 It is worth noticing that this law diﬀers from the one characterizing BEC in a uniform gas (see eqn (3.31)), where the T -dependence of the thermal component behaves like T 3/2 rather than T 3 . Like the uniform case, in the presence of harmonic trapping the ideal Bose gas also exhibits the saturation eﬀect discussed in Section 3.2, the number of NT = ζ(3)(kB T /ωho )3 of thermal atoms being independent of N in the BEC phase. In Section 13.5 we will show that interactions aﬀect this behaviour in an important way. Despite the rather simple nature of the model, results (10.10)–(10.11) are very important. In fact, they ﬁx the most important temperature scale of the problem. Typical values of the oscillator temperature ωho /kB in the available experiments with trapped gases of alkali atoms are a few nanokelvin, so that, for values of N ranging from 104 to 107 , one predicts critical temperatures ranging from 102 to 103 nK. The measured values of the transition temperature and of the temperature dependence of the condensate fraction were found to be very close to the predictions (10.10) and (10.11) of the ideal gas model. As an example, in Figure 10.1 we show the ﬁrst experimental results for N0 (T )/N obtained with rubidium atoms at Jila (Ensher et al., 1996). These results show explicitly the occurrence of a sudden transition at T ∼ Tc . It is interesting to compare this ﬁgure with the equivalent Figure 8.16 reporting the experimental results for the condensate fraction in superﬂuid 4 He. In Helium the condensate fraction approaches the value ∼ 0.1 at low temperatures, while the experimental results of Table 10.1 Values of the Riemann function ζ(n) = gn (1) for some values of n. n

ζ(n)

3/2

2

5/2

3

4

2.612

1.645

1.341

1.202

1.082

156

The Ideal Bose Gas in the Harmonic Trap

N0/N

1

0.5

0 0

0.6

1.2

1.8

T /T c0

Figure 10.1 Condensate fraction as a function of T /Tc0 . Circles represent the experimental results of Ensher et al. (1996), while the dashed line is eqn (10.11). The value of Tc0 is given c 1996, by eqn (10.10). Reprinted with permission from Physical Review Letters, 77, 4984; American Physical Society.

Figure 10.1 for a dilute gas clearly indicate that the condensate fraction tends to ∼ 1 when T → 0. The rather good agreement between the predictions of the ideal Bose gas model and experiments reﬂects the fact that the thermal component is very dilute and that result (10.11) is scarcely aﬀected by the inclusion of two-body interactions. Equations (10.10) and (10.11) are the predictions of the ideal gas model in the so-called semiclassical approximation, where the temperature of the gas is assumed to be much larger than the spacing between single-particle levels kB T ωk .

(10.12)

This condition was assumed in order to replace the sum over the single-particle states (10.8) with the integral (10.9). The comparison between (10.12) and the result (10.10) for the critical temperature shows that the BEC regime is compatible with the semiclassical approximation only if the natural condition N 1 is satisﬁed. This permits the approach to the thermodynamic limit, as we will discuss in Section 10.4.

10.2

Density of single-particle states and thermodynamics

The fact that the harmonic oscillator model predicts a temperature dependence for the condensate fraction which is diﬀerent from the corresponding law of uniform gases reﬂects the diﬀerent behaviour of the density of single-particle states. The density of states is deﬁned, in the semi-classical approximation, by the relation drdp g() = δ( − 0 (r, p)), (10.13) (2π)3 where 0 (r, p) = p2 /2m + Vext (r) is the classical energy corresponding to the singleparticle Hamiltonian (10.3). The concept of density of states is useful when the

Density of single-particle states and thermodynamics

157

discretized single-particle levels can be approximated with the continuum and consequently only if excitation energies relevant for the evaluation of the thermodynamic quantities satisfy the condition ωho . This is consistent with the semiclassical assumption (10.12). In a three-dimensional uniform gas, where Vext = 0, the density of states follows the law V m3/2 1/2 g() = √ . 23 π 2

(10.14)

Conversely, in the harmonic oscillator model one ﬁnds the result g() =

1 2 . 2(ωho )3

(10.15)

This explains the diﬀerent temperature dependence of the number NT of thermal particles which, below Tc , can be written as ∞ g() . (10.16) d β NT = e −1 0 The diﬀerent energy dependence exhibited by g() has its physical origin in the suppression of states in phase space due to the spatial conﬁnement produced by the oscillator potential. In this context it is interesting to discuss what happens if one reduces the dimensionality d of space. In fact, in two dimensions the uniform gas cannot exhibit the phenomenon of BEC at a ﬁnite temperature (see Section 7.4). In the uniform case the density of states behaves like g() ∼ d/2−1 and is constant for d = 2. As a consequence, the integral (10.16) exhibits an infrared logarithmic divergence which implies that the normalization condition NT ≤ N cannot be satisﬁed at any ﬁnite temperature. The situation is diﬀerent in the presence of harmonic trapping, where the energy dependence is given by g() =

1 d−1 , $d (d − 1)! x=1 ωk

(10.17)

and is linear in for d = 2. The above consideration permits us to conclude that the harmonically trapped ideal Bose gas also exhibits the phenomenon of BEC in two dimensions, where one ﬁnds the result kB Tc (d = 2) = π 2 /6ωho N 1/2 . One should however keep in mind that this result is fragile with respect to the inclusion of two-body interactions. Actually, at ﬁnite temperatures the physics of Bose–Einstein condensation in two dimensions is strongly inﬂuenced by the presence of dynamic correlations, as we will discuss in Chapter 23. In terms of the density of states one can easily calculate all the relevant thermodynamic functions. For example, the value of the chemical potential of the gas trapped in the three-dimensional oscillator is ﬁxed by the relation (z = eβμ ) N=

kB T ωho

3 g3 (z)

(10.18)

158

The Ideal Bose Gas in the Harmonic Trap

above Tc . Below Tc one has instead z = 1. The total energy of the gas is also easily calculated. One ﬁnds: E(T ) =

∞

d 0

g() = 3kB T z −1 eβ − 1

kB T ωho

3 g4 (z),

(10.19)

with z ﬁxed by the solution of (10.18). Starting from the energy one can evaluate all the other thermodynamic quantities. In particular, it is easy to show, using the recurrence relation (3.27) obeyed by the Bose functions, that the speciﬁc heat at constant volume exhibits the discontinuity ΔCV = CV (T = Tc+ ) − CV (T = Tc− ) = −9

ζ(3) N kB ζ(2)

(10.20)

at the critical point. Another important quantity is the entropy. Starting from the ideal gas expression (3.16) or, equivalently, from result (10.19) for the energy, one ﬁnds that the entropy of the three-dimensional harmonically trapped gas is given by the expression

g4 (z) S(T ) = kB NT 4 − ln z , (10.21) g3 (z) where NT = N (T /Tc )3 is the number of atoms out of the condensate (NT = N above Tc ). Below Tc one has: 4 E(T ) = 4kB S(T ) = 3 T

10.3

kB T ωho

3 g4 (1).

(10.22)

Density and momentum distribution

In a nonuniform gas it is important to discuss the behaviour of the diagonal density, which is given, for T ≤ Tc , by the sum n(r) = n0 (r) + nT (r)

(10.23)

of the condensate and of the thermal densities. The density (10.23) is normalized to the total number of particles: drn(r) = N . Notice that only the total density is measured in experiments. In the ideal gas model the condensate density is given by n0 (r) = N0 |ϕ0 (r)|2 ,

(10.24)

where ϕ0 is the ground state wave function (10.5) of the oscillator, while the thermal density nT (r) can be calculated using the semiclassical expression nT (r) =

dp np (r), (2π)3

(10.25)

Density and momentum distribution

159

where np (r) =

1 exp [β ((r, p) − μ)] − 1

(10.26)

is the particle distribution function. Below Tc one has μ = 0 and the integration (10.25) in momentum space gives nT (r) =

1 g3/2 (e−βVext ), λ3T

(10.27)

where g3/2 (z) is the Bose function (3.26) with p = 3/2, and λT = 2π2 /mkB T is the thermal wavelength. In Figure 10.2 we show the condensate and the thermal density calculated at the temperature T = 0.9Tc for a system of N = 5000 particles. The curves correspond to the column density, namely the particle density integrated along one direction, n(z) = dxn(x, 0, z). This is a typical measured quantity, the x being the direction of the light beam used to image the atomic cloud. The ﬁgure clearly shows that the thermal and condensate densities are well separated in space. In fact, the average square radius of the thermal cloud in the kth direction scales like rk2 T = (ζ(4)/ζ(3))kB T /2mωk2 , while the one of the condensate scales as rk2 0 = /(2mωk ). The ratio between the two square widths rk2 T ζ(4) kB T = rk2 0 ζ(3) ωk

(10.28)

is a large number since we always assume kB T ωk . The separation in space between the condensate and the thermal component is a unique feature exhibited by nonuniform

Column density

400 n0 200

nT 0 −8

−4

0 z

4

8

Figure 10.2 Column density for 5000 noninteracting bosons in a spherical trap at temperature T = 0.9 Tc0 . The central peak is the condensate superimposed onto a broader thermal distribution. Distance and density are in units of aho and a−2 ho , respectively. The density is normalized to the number of atoms.

160

The Ideal Bose Gas in the Harmonic Trap

Bose gases and permits us to reveal the phenomenon of BEC by simply taking images of the sample in real space. This explains why the experimental realization of cold bosons conﬁned in harmonic traps has rapidly made a spectacular impact in the study of Bose–Einstein condensation. One should not however forget that estimate (10.28) is based on the ideal gas model and that the ratio between the two widths is signiﬁcantly smaller after inclusion of the interaction (see Chapter 11). Let us now discuss the behaviour of the trapped gas in momentum space. The momentum distribution is given by the sum n(p) = n0 (p) + nT (p)

(10.29)

of the condensate and of the thermal components, and is normalized to the total number of particles: dpn(p) = N . The condensate contribution is easily evaluated by taking the Fourier transform of the ground state wave function (10.5). One ﬁnds: n0 (p) = N0 |ϕ0 (p)| = N0 2

1 πmωho

3/2

1 exp − m

p2y p2 p2x + + z ωx ωy ωz

while the thermal contribution takes the form 2 dr 1 nT (p) = np (r) = g3/2 (e−βp /2m ). 3 3 (2π) (λT mωho )

,

(10.30)

(10.31)

Once more one recognizes a clean separation between the two components. In fact, the average square momentum of the condensate in the kth direction is given by p2k 0 = mωk /2, while that of the thermal cloud is independent of the direction and is given by p2k T = (ζ(4)/ζ(3))mkB T /2. The ratio ζ(4) kB T p2k T = p2k 0 ζ(3) ωk

(10.32)

between the two square widths coincides with the corresponding ratio (10.28) in coordinate space. This result is the consequence of the harmonic shape of trapping and is modiﬁed by the inclusion of two-body interactions as we will show in the next section. The net separation between the condensate and the thermal components in momentum space is not peculiar to the trapped gas and is also exhibited by uniform systems, where the momentum distribution of the condensate reduces to a delta function (see Chapter 2). Actually, in uniform systems the investigation of the momentum distribution is the only way to detect directly the phenomenon of Bose–Einstein condensation, as discussed in Section 8.5 in the case of superﬂuid helium. It is ﬁnally worth discussing the above results in terms of the Heisenberg uncertainty inequality Δrk Δpk ≥

1 , 2

(10.33)

Release of the trap and expansion of the gas

161

where Δrk ≡ rk2 and Δpk ≡ p2k are the usual widths. For the condensate one ﬁnds that the inequality (10.33) reduces to an equality, as a consequence of the Gaussian form of the wave function. For the thermal cloud one instead ﬁnds the result Δrk Δpk =

1 ζ(4) kB T , 2 ζ(3) ωk

(10.34)

which, because of the semiclassical condition kB T ωk used to derive the above results, is always much larger than .

10.4

Thermodynamic limit

In the previous sections we have systematically made the assumption that the sum over the discretized levels can be replaced by an integral. This is equivalent to employing the semiclassical expression (10.13) for the density of states. This approximation is clearly related to the concept of the thermodynamic limit. In uniform systems the thermodynamic limit is obtained by letting the number N of particles and the volume V tend to inﬁnity, the ratio N/V being kept constant. In a harmonically trapped gas the density is not uniform and consequently the thermodynamic limit should be deﬁned in a diﬀerent way. In the following we will use a procedure in which we let N tend 3 to inﬁnity and ωho to zero, the combination N ωho being kept constant. In this limit the semiclassical condition (10.12) is automatically fulﬁlled and the critical temperature (10.10) and the condensate fraction (10.11) take a well-deﬁned value. This procedure implies that the central value of the density of the condensate N (mωho /π)3/2 exhibits a divergent behaviour in the thermodynamic limit. In contrast, the central value of the thermal density remains constant. This asymmetric behaviour between the condensate and the thermal component in coordinate space is the consequence of the harmonic trapping and is exhibited in momentum space as well. It is interesting to compare these results with the behaviour of the condensate in the uniform gas (see Chapter 3). In this case the condensate component exhibits the well-known δ-peak structure (3.46) in momentum space, but is of course uniform in coordinate space.

10.5

Release of the trap and expansion of the gas

Much experimental information on Bose–Einstein condensation in trapped gases is provided by imaging the density of the atomic cloud after switching oﬀ the conﬁning trap. These experiments are important because the direct in situ imaging is not always feasible. In the case of the ideal gas the expansion can be described analytically. In fact, employing the Heisenberg time evolution formalism, one can write the general result ϕ0 (r, t) = e−3iπ/4

m 3/2 m (r − r )2 dr ϕ0 (r ) exp i 2πt 2t

(10.35)

162

The Ideal Bose Gas in the Harmonic Trap

which can be easily proven to satisfy the Schr¨ odinger equation with the initial condition ϕ0 (r, 0) = ϕ0 (r). By using the Gaussian choice for ϕ0 at t = 0, one ﬁnds that the condensate function, after releasing the harmonic trap, expands according to the law

mω 3/4 % 1 mωk 1 − iωk t 2 ho ϕ0 (r, t) = exp − rk . (10.36) 2 2 π 2 1 + ωk t (1 + iωk t)1/2 k = x,y,z

The wave function has a real and an imaginary part. The time dependence of the condensate density is given by

mω 3/2 % mωk 1 ho 2 r n0 (r, t) = N0 exp − , (10.37) π (1 + ωk2 t2 ) k (1 + ωk2 t2 )1/2 k = x,y,z

while the velocity ﬁeld v = −i(ϕ∗0 ∇ϕ0 − ϕ0 ∇ϕ∗0 )/(2m|ϕ0 |2 ) takes the simple form vk (r, t) =

ωk2 t rk 1 + ωk2 t2

(10.38)

and approaches the classical law v = r/t for large times. The momentum distribution instead remains equal to its initial value (10.30) due to the absence of interactions. Let us now discuss the behaviour of the expansion of the thermal cloud. The distribution function (10.26), after the release of the trap, evolves in time according to the law p np (r, t) = np r − t , (10.39) m from which one can easily calculate the time dependence of the thermal density nT (r, t) = dpnp (r, p, t). One ﬁnds the result nT (r, t) =

1 g3/2 (˜ z (r, t)) λ3T

% k = x,y,z

1 , (1 + ωk2 t2 )1/2

(10.40)

where z˜(r, t) = exp[−β V˜ext (r, t)] and ωk2 1 V˜ext (r, t) = m r2 2 1 + ωk2 t2 k

(10.41)

k=x,y,z

plays the role of an eﬀective potential, characterizing, at each instant, the shape of the thermal density. For times much larger than the inverse of the oscillator frequencies (ωk t 1) the density proﬁles (10.37) and (10.40) are proportional to the momentum distributions (10.30) and (10.31), respectively. In fact, both the condensate and the thermal density distributions approach, in this limit, the value n0,T (r, t) →

m 3 t

n0,T (p),

(10.42)

Bose–Einstein condensation in deformed traps

163

where, in the right-hand side, the momentum distribution should be calculated at the value p = mr/t. It is worth pointing out that the asymptotic shape of the thermal density is isotropic, consistent with the isotropy of its momentum distribution. In contrast, the asymptotic shape of the condensate density (10.37) exhibits the characteristic deformation of the initial momentum distribution (10.30). The above results hold only in the noninteracting model and are modiﬁed by the inclusion of two-body interactions (see Section 12.7).

10.6

Bose–Einstein condensation in deformed traps

In the previous section we have derived our results making a general choice for the trapping frequencies. Since most of the available traps are not isotropic it is important to discuss explicitly the eﬀects of the deformation. Interesting quantities are the widths of the density and of the momentum distributions. Let us ﬁrst consider the condensate. In coordinate and momentum space we ﬁnd, respectively, the results rk2 0 ω = 2 r 0 ωk

(10.43)

ωk p2k 0 = , p2 0 ω

(10.44)

and

with k, = x, y, z. The above results show that the ratio of the square radii in coordinate space scales like the inverse of the trapping frequencies, while in momentum space the ratio scales linearly. The situation is diﬀerent for the thermal component, where the ratio in coordinate space is given by rk2 T ω2 = , r2 T ωk2

(10.45)

while in momentum space it is independent of the deformation: p2k T = 1. p2 T

(10.46)

Result (10.46) reﬂects the isotropy of the momentum distribution of the thermal cloud. The observation of anisotropy in momentum space in the presence of a deformed trap would consequently provide an important signature of Bose–Einstein condensation, as explicitly pointed out in the ﬁrst experiments carried out at Jila (Anderson et al. 1995). Once more, one should not forget that the above results ignore the presence of two-body interactions. Interactions do not signiﬁcantly modify the distribution of the thermal cloud, but they have a crucial eﬀect on the condensate. Furthermore, the momentum distribution of the condensate cannot simply be measured by looking at the expansion of the gas following the sudden switching oﬀ of the trap, since interactions modify the mechanism of the expansion of the condensate. Alternative methods to measure the momentum distribution will be discussed in Chapter 12.

164

10.7

The Ideal Bose Gas in the Harmonic Trap

Adiabatic formation of BEC with non-harmonic traps

As shown by eqn (10.10), the critical temperature in the harmonic oscillator model depends explicitly on the trapping frequency. One could imagine that, starting from an initial conﬁguration above Tc , a possible route to BEC may be achieved by increasing adiabatically the value of ωho and hence of Tc , thereby bringing the system into the BEC phase. This possibility is ruled out by the fact that the entropy of the gas in the harmonic oscillator model is a universal function of the ratio kB T /ωho . This can easily be checked by looking at expression (10.21) for the entropy of the three-dimensional harmonically trapped gas. In fact, in this case both z and NT depend on the ratio kB T /ωho . In conclusion, any adiabatic transformation which increases ωho will also increase the temperature by leaving the ratio T /Tc unchanged. The possibility of reaching BEC via an adiabatic transformation is not, however, excluded if, instead of changing the oscillator frequency, one changes adiabatically the shape of the potential. This possibility is illustrated in Figure 10.3. Let us suppose that at the time t = 0 the gas is conﬁned in a harmonic potential above Tc0 . According to the discussions of Section 3.1 this means that the chemical potential is smaller than the energy of the lowest single-particle state, here approximated with the bottom of the potential. If we now switch on adiabatically a narrow potential producing a bound state with energy −U we may eventually fulﬁl the condition μ = −U . As a consequence, the gas, which was initially normal, will start exhibiting the phenomenon of Bose–Einstein condensation and the new lowest state will be occupied macroscopically. In the ideal gas model one can easily calculate the condensate fraction as a function of the well depth U . We will assume that the potential is suﬃciently narrow not to perturb the level distribution of the thermal cloud, which will consequently be described as a harmonically trapped gas. In the presence of BEC the fugacity

V(r)

V(r)

U μ

μ

Figure 10.3 By adding an optical trap to a magnetic trap it is possible to produce BEC in an adiabatic way. Prior to deformation the magnetic trap contains a gas above BEC with μ < 0. When a potential well with depth −μ is added adiabatically a small condensate forms.

Adiabatic formation of BEC with non-harmonic traps

165

takes the value z = e−U/kB T , so that the number of atoms in the thermal cloud is given by

∞

NT = 0

g() = d −1 β z e −1

kB T ωho

3

g3 (e−U/kB T ),

(10.47)

where we have used the harmonic expression (10.15) for the density of states. By setting (10.47) equal to N one obtains the new value of the critical temperature, which will, of course, be larger than the original value (10.10). Let us suppose, for simplicity, that gas temperature is initially slightly above Tc0 . This implies that the entropy is obtained by setting NT = N and z = 1 in eqn (10.21): g4 (1) S . = N4 kB g3 (1)

(10.48)

After adding the narrow potential the chemical potential will take the value μ = −U and hence z = e−U/kB T . As a consequence, the entropy will be given by the expression (see eqn (10.21))

S U g4 (e−U/kB T ) , + = NT 4 kB g3 (e−U/kB T ) kB T

(10.49)

with NT given by eqn (10.47). By imposing that the entropies calculated before and after adding the potential are the same (adiabaticity condition), one can determine the ﬁnal value of T and hence of NT . In Figure 10.4 we show the behaviour of the

N0/N

0.4

0.2

0 0

2

4

U/kBTc0

Figure 10.4 Adiabatic formation of the condensate in a nonharmonic trap. Condensate fraction as a function of the depth of the optical potential. The initial temperature has been assumed to be equal to the critical temperature Tc0 calculated in the magnetic trap.

166

The Ideal Bose Gas in the Harmonic Trap

condensate fraction N0 /N as a function of the ratio U/kB Tc0 , with Tc0 given by (10.10). The ﬁgure clearly shows that by increasing the value of U one can produce more and more degenerate conﬁgurations. The adiabatic realization of Bose–Einstein condensation has been experimentally demonstrated by Stamper-Kurn et al. (1998b), by applying a red-detuned laser ﬁeld to a non-condensed Bose gas conﬁned in a magnetic trap. In this experiment the role of two-body interactions is however rather important, and the ideal gas model developed above provides only a semi-quantitative description of the observed results. Another example of adiabatic formation of Bose–Einstein condensation is provided by the adiabatic transfer of entropy between two distinguishable atomic gases conﬁned by diﬀerent harmonic potentials. This experiment was realized by Catani et al. (2009) with a mixture of 87 Rb and 41 K atoms. The adiabatic compression (increase of ωho ) of the harmonic potential conﬁning Potassium atoms results in an increase of their critical temperature Tc = 0.94ωho N 1/3 . The temperature of these atoms instead remains almost constant because of the presence of the Rubidium gas, which plays the role of a thermal reservoir to which Potassium atoms transfer part of their entropy. The net result is an increase of quantum degeneracy of Potassium atoms, which can eventually exhibit Bose–Einstein condensation, even if initially their temperature was above Tc (see Figure 10.5). The ﬁgure also shows the comparison between the measured

0.30

K BEC fraction

2.8 0.20

(a)

(b) 3.0

0.15 3.2

0.10 0.05

3.4

0.00

3.6 120

140

180 200 160 K harmonic frequency (Hz)

K entropy per particle, S/N (kB)

2.6 0.25

220

Figure 10.5 Formation of BEC in a Potassium (K) gas by adiabatic compression and entropy transfer to a Rubidium (Rb) gas. Data (circles) are compared to the theoretical prediction (solid line) based on eqn (10.50). The inset displays absorption images of the K sample before (a) and after (b) the compression. From Catani et al. (2009). Reprinted with c 2009, American Physical Society. permission from Physical Review Letters, 103, 140401;

Adiabatic formation of BEC with non-harmonic traps

167

condensate fraction of Potassium atoms and the theoretical prediction based on the conservation of the total entropy of the system S(Ti , ωK,i ) + S(Ti , ωRb ) = S(Tf , ωK,f ) + S(Tf , ωRb ),

(10.50)

calculated before (i) and after (f ) the compression of the Potassium harmonic trap. Equation (10.50) permits us to determine the actual ﬁnal temperature Tf of the two gases. In the theoretical analysis of Figure 10.5 the ideal gas expressions (10.21) and (10.22) for the entropy of the two atomic species above and below TC were employed.

11 Ground State of a Trapped Condensate In this chapter we apply the general formalism developed in Chapter 4 for nonuniform gases to investigate the ground state of N interacting bosons conﬁned by an external potential. In particular, we discuss the predictions of the Gross-Pitaevskii equation (5.18) 2 2 ∇ − + Vext (r) + g|Ψ0 (r)|2 Ψ0 (r) = μ0 Ψ0 (r) 2m

(11.1)

for the order parameter, with special emphasis on the case of harmonic conﬁnement. In eqn (11.1) g = 4π2 a/m is the relevant coupling constant of the problem, ﬁxed by the s-wave scattering length a. In the absence of two-body interactions (g = 0) this equation reduces to the usual single-particle Schr¨ odinger equation and, due√to the assumption made for the normalization of the order parameter, one has Ψ0 = N ϕ0 , where ϕ0 is the ground state wave function of the single-particle Hamiltonian (10.3), normalized to unity. In this chapter we will consider real solutions for the order par√ ameter, which can be hence identiﬁed as the square root of the density: Ψ0 = n. It is worth stressing that this is not the most general situation. In fact, one can also ﬁnd stationary solutions of the Gross-Pitaevskii equation corresponding to complex functions for the order parameter. In this case the solutions are associated with stationary currents, as happens for the vortical conﬁgurations discussed in Section 5.3. The main emphasis of this chapter is to point out how the combined eﬀect of Bose–Einstein condensation, nonuniform conﬁnement, and two-body interactions characterize the ground state properties of the system, which are signiﬁcantly modiﬁed with respect to the predictions of the ideal gas model of Chapter 10. Many of the physical quantities discussed in this chapter can be measured with good accuracy and consequently their investigation provides an important test of Gross-Pitaevskii theory.

11.1

An instructive example: the box potential

In this section we discuss the insightful problem in which N interacting bosons are conﬁned by a potential of the form Vext = 0 for 0 < z < L and +∞ outside. This potential corresponds to imposing the boundary condition Ψ0 = 0 on the planes z = 0

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

An instructive example: the box potential

169

and z = L. In the absence of two-body interactions the order parameter relative to the ground state takes the form √ πz , (11.2) Ψ0 (r) = 2n sin L where n = N/V is the average density, V is the volume of the box, and, to simplify the discussion, we have considered cyclic boundary conditions along the x and y directions. The resulting density proﬁle n = |Ψ0 |2 has been shown in Figure 3.5. One can see that the boundary produces a highly inhomogeneous proﬁle, the density varying on distances ﬁxed by the size L of the system. The eﬀect of two-body interactions on the density proﬁle is spectacular. In fact, the system gains a macroscopic amount of energy by making the density uniform in the interior of the box. The solution of the Gross-Pitaevskii equation (11.1) near √ z = 0 is easily obtained by rescaling the wave ˜ 0 = Ψ0 / n and by introducing the dimensionless variable function according to Ψ z˜ = z/ξ, where 2 (11.3) ξ= 2mgn is the healing length evaluated at the average density n = n. As a result of the above transformations the Gross-Pitaevskii equation takes the dimensionless form −

d2 ˜ ˜ 3 (˜ ˜ z ). z) + Ψ Ψ0 (˜ 0 z ) = Ψ0 (˜ d˜ z2

(11.4)

˜ 0 (0) = 0 Assuming L ξ, the boundary conditions for the solution of (11.4) become Ψ ˜ and Ψ0 (˜ z ) = 1 for z˜ 1. The solution of the Gross-Pitaevskii equation (11.1) then takes the simple form in the region z L √ z (11.5) Ψ0 (z) = n tanh √ , 2ξ √ ¯ in an interval of the order showing that the order parameter diﬀers from the value n of the healing length ξ near z = 0. Analogously, one can characterize the behaviour of Ψ0 near the plane z = L. The healing length ξ then emerges as a crucial parameter of the theory, characterizing the interacting nature of the system. By increasing the size of the coupling constant g, the value of ξ reduces and consequently the region where the density varies in space is increasingly compressed. In this case ξ L and the system, as a whole, can be considered uniform (see Figure 3.5). In this limit the kinetic energy term in the Gross-Pitaevskii equation (11.1) can be neglected everywhere except near the boundary. In contrast, if ξ becomes comparable to L then the boundary conditions inﬂuence the solution in the whole interval 0 < z < L. The above discussion reveals that two-body interactions can signiﬁcantly modify the ground state proﬁle of a Bose– Einstein condensate. Of course, the ﬁnal result depends crucially on the actual form of the trapping potential and new, interesting scenarios emerge in the case of harmonic trapping, as we will extensively discuss in the following sections.

170

11.2

Ground State of a Trapped Condensate

Interacting condensates in harmonic traps: density and momentum distribution

In the presence of harmonic trapping Vext (r) =

m 2 2 m 2 2 m 2 2 ω x + ωy y + ωz z , 2 x 2 2

(11.6)

the Gross-Pitaevskii (11.1) equation should be solved numerically, except in some important limits. The physical consequence of the interaction on the solution of the equation is very clear. If the interaction is repulsive (g > 0) the gas will expand and the size of the cloud will increase with respect to the noninteracting case. Notice that this eﬀect does not take place in the case of the inﬁnite wall potential, where the size of the system is ﬁxed by the length L of the box. Eventually, if the eﬀect of the interaction is very important, the width of the gas will become so large and the density proﬁle so smooth that one can ignore the kinetic energy term in the Gross-Pitaevskii equation. The eﬀect of the kinetic energy term is, in fact, proportional to the gradient of the order parameter and hence of the density. The limit in which one ignores the kinetic energy term in the Gross-Pitaevskii equation (11.1) iscalled the Thomas–Fermi limit and is characterized by the analytic solution ΨT F = n0T F (r), with n0T F (r) =

1 0 (μ − Vext (r)) g TF

(11.7)

if μ0T F > Vext and zero elsewhere (Baym and Pethick, 1996). The value of the chemical potential entering eqn (11.7) is ﬁxed by imposing the proper normalization to the density and takes the value 2/5 ωho 15N a 0 μT F = , (11.8) 2 aho where aho = /(mωho ) is the oscillator length associated with the geometrical average ωho = (ωx ωy ωz )1/3 of the three oscillator frequencies. By integrating the thermodynamic relation μ = ∂E/∂N one also obtains the Thomas–Fermi result ET0 F 5 = μ0T F N 7

(11.9)

for the total energy per particle. The transition between the ideal gas and the Thomas–Fermi limit takes place in a smooth way by varying the relevant parameters of the problem. It is interesting to identify the proper combination of parameters which characterizes this transition. This can easily be found by rewriting the Gross-Pitaevskii equation in dimensionless variables. Let us consider, for simplicity, a spherical harmonic trap with frequency ωho and let us use aho and ωho as units for lengths and energies respectively. By labelling the rescaled variables with a tilde, the Gross-Pitaevskii equation becomes

˜ r) = 2˜ ˜ r), ˜ 2 (˜r) Ψ(˜ ˜ 2 + r˜2 + 8πN a Ψ −∇ μΨ(˜ (11.10) aho

Interacting condensates in harmonic traps: density and momentum distribution

171

−3/2

˜ = N −1/2 a where Ψ ho Ψ0 . In these units the order parameter satisﬁes the ˜ 2 = 1. It is now evident that the importance of the normalization condition d˜r|Ψ| atom–atom interaction is completely ﬁxed by the combination N a/aho , hereafter called the Thomas–Fermi parameter. The Thomas–Fermi approximation is valid if this parameter is very large: N

a 1. aho

(11.11)

Typical values of a/aho are of the order of 10−3 in standard experimental conﬁgurations, so that for samples containing more than 105 atoms the Thomas–Fermi parameter is indeed very large. To illustrate the transition from the noninteracting model to the Thomas–Fermi limit we show in Figure 11.1 some typical results for the wave function Ψ0 calculated by solving the Gross-Pitaevskii eqn (11.1) with diﬀerent values of N a/aho . The eﬀects of the interaction are revealed by the deviations from the Gaussian proﬁle predicted by the noninteracting model. For large values of the Thomas–Fermi parameter the solution of the equation becomes broader and broader and, consequently, the density is smaller and smaller. Excellent agreement is found by comparing the solution of the Gross-Pitaevskii equation with the experimental density proﬁles obtained at low temperature (see Figure 11.2). The comparison reveals the crucial role played by twobody interactions in characterizing the shape of the density proﬁle of the ground states of these harmonically trapped Bose gases. The density proﬁle, in the Thomas–Fermi limit, takes the form of an inverted parabola (see eqn (11.7)) which vanishes at the classical turning point, characterized

a>0

Wave function

0.4 1

0.2

10 100

0 0

2

4

6

r/aho

Figure 11.1 Condensate function, at T = 0, obtained by solving numerically the stationary Gross–Pitaevskii eqn (11.1) in a spherical trap with repulsive interaction. The three solid lines correspond to N a/aho = 1, 10, and 100. The dashed line is the prediction of the ideal gas. The curves are normalized to 1 (see eqn (11.10)). From Dalfovo et al. (1999).

172

Ground State of a Trapped Condensate

Column density [μm−2]

1000 800 600 400 200 0 −40

0 z [μm]

40

Figure 11.2 Density distribution of 80 000 sodium atoms in the trap of Hau et al. (1998) as a function of the axial coordinate. The experimental points correspond to the measured optical density. The solid line is the prediction of GP theory, while the dashed line is the prediction of the noninteracting gas. From Dalfovo et al. (1999).

by the three radii Rk of the ellipsoid (k = x, y, z). The value of these radii is ﬁxed by the oscillator frequencies according to the relation μ0T F =

1 1 1 mωx2 Rx2 = mωy2 Ry2 = mωz2 Rz2 . 2 2 2

(11.12)

Using the Thomas–Fermi expression (11.8) for the chemical potential, the radii Rk can be written as Rk = aho

15N a aho

1/5

ωho , ωk

(11.13)

and reduce, in the case of isotropic trapping, to R = aho

15N a aho

1/5 .

(11.14)

With respect to the ideal gas, where the size of the condensate is ﬁxed by the oscillator length and is independent of N , in the Thomas–Fermi limit the size increases like N 1/5 . As with the case of the box potential (see Section 11.1) it is useful to discuss the conditions of applicability of the Thomas–Fermi approximation in terms of the healing length (11.3). This quantity, evaluated in the centre of the trap where the density takes the value n0T F (0) = μ/g (see eqn (11.7)), obeys the relationship ξ = R

a2ho R

2

=

15N a aho

−2/5 ,

(11.15)

Energy, chemical potential, and virial theorem

173

showing that, in the Thomas–Fermi limit N a/aho 1, the healing length becomes much smaller than the size of the condensate. This is the analogue of the condition ξ L discussed in Section 11.1. The average square radii rk2 = (1/N ) drrk2 n0T F in the Thomas–Fermi approximation are simply given by rk2 = (1/7)R2k and consequently scale as the inverse of the square of the trapping frequencies: ω2 rk2 = . r2 ωk2

(11.16)

This result diﬀers from the case of the ideal Bose gas, where they instead scale like the inverse of the corresponding frequencies (see eqn (10.43). The increase of the size of the condensate implies a reduction of the value of the density in the centre of the trap. Actually, the Thomas–Fermi value n0T F (0) = μ/g is much lower than the one predicted for noninteracting particles, where nho (0) = N (mωho /π)3/2 (see eqn (10.5)). The ratio between the central densities evaluated in the two limits is given by the expression 152/5 π 1/2 n0T F (0) = nho (0) 8

Na aho

−3/5 .

(11.17)

Also, the momentum distribution of the condensate can be evaluated analytically in the Thomas–Fermi limit. By taking the Fourier transform of the Thomas–Fermi wave function ΨT F = (μ − Vext )/g, one ﬁnds the result (Baym and Pethick, 1996) nT F (p) = N

15 3 R 163

p) J2 (˜ p˜2

2 ,

(11.18)

where R =# (Rx Ry Rz )1/3 is given by eqn (11.14), J2 is the Bessel function of order 2, and p˜ = p2x Rx2 + p2y R2y + p2z Rz2 / is the dimensionless momentum variable. Equation (11.18) explicitly shows that the width of the momentum distribution in the kth direction scales as 1/Rk and is consequently much narrower than the width predicted by the noninteracting gas, which is instead ﬁxed by the inverse of the oscillator length (see eqn 10.30). In the limit of a large sample, corresponding to a very smooth density proﬁle, the momentum distribution of the condensate approaches a delta function, a typical feature of uniform Bose–Einstein condensed systems.

11.3

Energy, chemical potential, and virial theorem

It is worth noticing that the stationary solution of the Gross-Pitaevskii eqn (11.1) minimizes the energy functional (5.8) for a ﬁxed number of particles. Since we consider stationary solutions without current terms, the energy becomes a functional of the density only and can be written in the form

2 √ gn2 E(n) = dr | ∇ n |2 +nVext + . (11.19) 2m 2

174

Ground State of a Trapped Condensate

The ﬁrst term corresponds to the quantum kinetic energy √ 2 | ∇ n |2 Ekin = dr 2m

(11.20)

and is usually named quantum pressure. It vanishes for uniform systems and its contribution to the total energy becomes less and less important as the Thomas–Fermi parameter N a/aho increases. The mean ﬁeld kinetic energy (11.20) should not be confused with the true kinetic energy of the gas, which is sensitive to the microscopic details of the two-body interaction (see Section 4.3) and cannot be calculated within Gross-Pitaevskii theory. It accounts for the macroscopic component of the kinetic energy associated with the condensate wave function. The second and third terms are, respectively, the harmonic oscillator energy Eho = drnVext (11.21) and the two-body interaction energy Eint =

g 2

drn2 .

(11.22)

By direct integration of the GP equation (11.1) one ﬁnds the useful expression μ0 =

1 (Ekin + Eho + 2Eint ) N

(11.23)

for the chemical potential in terms of the diﬀerent contributions to the energy. A further important relationship can be found by means of the virial theorem. In fact, since the energy functional (5.7) is stationary for any variation of the function of Ψ around the solution Ψ0 of the Gross-Pitaevskii eqn (11.1), one can choose a scaling transformation of the form Ψ(x, y, z) = (1 + ν)3/2 Ψ0 [(1 + ν)x, (1 + ν)y, (1 + ν)z], corresponding to n(x, y, z) = (1 + ν)3 n0 [(1 + ν)x, (1 + ν)y, (1 + ν)z)]. By inserting this transformation into (11.19) and imposing that the energy variation vanishes at ﬁrst order in ν, one obtains the identity 2Ekin − 2Eho + 3Eint = 0,

(11.24)

also known as the virial relation. It is worth noticing that results (11.23)–(11.24) are exact within the Gross-Pitaevskii theory and hold for any value of the parameter N a/aho , including the case of negative a. In addition to the energy and to the chemical potential it is useful to discuss the so-called release, or internal energy, deﬁned by the expression Erel = Ekin + Eint .

(11.25)

The release energy can be measured by imaging the gas after the sudden switching oﬀ of the trap and measuring the asymptotic velocity distribution of the expanding gas.

Finite-size corrections to the Thomas–Fermi limit

175

Uint (nK)

200

100

0

0

2 4 Number of condensed atoms N0 (106)

Figure 11.3 Release energy of the condensate as a function of the number of condensed atoms in the MIT trap with sodium atoms. For these condensates the initial kinetic energy is negligible and the release energy coincides with the mean-ﬁeld energy. The symbol Uint is used here for the mean-ﬁeld energy per particle. Triangles—clouds with no visible thermal component; circles—clouds with both thermal and condensed fractions visible. The solid line 2/5 is a ﬁt proportional to N0 . From Mewes et al. (1996). Reprinted with permission from c 1996, American Physical Society. Physical Review Letters, 77, 416;

During the ﬁrst phase of the expansion both the quantum kinetic energy (quantum pressure) and the interaction energy are rapidly converted into kinetic energy of motion. Then the atoms expand at constant velocity. Since energy is conserved during the expansion, its initial value (11.25), calculated with the stationary GP equation, can be compared directly with experiments. The above discussion clearly reveals that these experiments do not measure the initial kinetic energy of the trapped gas as would happen in the noninteracting case, where Eint = 0. Rather, especially when the Thomas–Fermi parameter is large, they are mainly sensitive to the interaction energy Eint . The experimental analysis of the release energy (Mewes et al., 1996; Holland et al., 1997) has actually provided clear evidence of the crucial role played by two-body interactions. In fact, the noninteracting model predicts that the release energy per particle is Erel /N = (1/2)(ωx + ωy + ωz ), independent of N . Conversely, the observed release energy depends rather strongly on N , in good agreement with the theoretical predictions obtained for the interacting gas. In Figure 11.3 we show the experimental data of Mewes et al. (1996), which explicitly reveal the N 2/5 dependence predicted in the Thomas–Fermi limit.

11.4

Finite-size corrections to the Thomas–Fermi limit

In the preceding sections we have shown that, when the Thomas–Fermi parameter N a/aho is large and positive, the solution of the GP equation approaches the analytic solution (11.7) and the chemical potential takes the value (11.8). This limit corresponds

176

Ground State of a Trapped Condensate

to neglecting the quantum pressure term in the solution of the GP equation. Using eqns (11.23) and (11.24) one then obtains the useful asymptotic results for the oscillator and interaction energies: Eho /N = (3/7)μ0T F and Eint /N = (2/7)μ0T F , with μ0T F given by eqn (11.8). In the Thomas–Fermi limit the main contribution to the integrals (11.21) and (11.22) for Eho and Eint arises from the central region, where the density diﬀers from zero and varies smoothly. This explains why the kinetic energy (11.20), which is sensitive to the surface region, is vanishingly small in this limit. An important question is how to calculate the kinetic energy when the Thomas–Fermi parameter N a/aho becomes large. It would be wrong to estimate Ekin by inserting the Thomas– Fermi proﬁle (11.7) into eqn (11.20). In fact, the integral would exhibit a divergent behaviour near the classical boundary, where nT F vanishes. Actually, the region where Vext ∼ μ is not correctly accounted for by the Thomas–Fermi approximation and its proper description requires the explicit inclusion of quantum eﬀects. This unphysical divergent behaviour is also reﬂected in the large p behaviour of the Thomas–Fermi momentum distribution (11.18), which behaves like 1/p5 , yielding a divergence in the kinetic energy integral dpn(p)p2 /2m. We will now discuss the proper description of the solution of the Gross-Pitaevskii equation near the classical boundary region, which allows for the explicit calculation of the kinetic energy in the Thomas–Fermi limit. With respect to similar procedures used in the study of the Schr¨ odinger equation in the presence of an external ﬁeld, the present method (Dalfovo et al., 1996) explicitly includes the interatomic forces which are responsible for crucial nonlinear eﬀects in the equations of motion. Let us consider, for simplicity, a spherical trap. The Gross-Pitaevskii eqn (11.1) takes the form −

2 d2 2 d Ψ0 + [Vext (r) − μ]Ψ0 + gΨ30 = 0. Ψ0 − 2 2m dr mr dr

(11.26)

Let R be the boundary of the system, determined by the equation μ = Vext (R). The value of R is given by the Thomas–Fermi expression (11.14). Near this point, where |r − R| R, one can carry out the linear ramp expansion for the external potential: Vext (r) − μ = (r − R)F,

(11.27)

where F is the modulus of the attractive external force F = −∇Vext , evaluated at r = R. Moreover, for values of R much larger than the thickness of the boundary (see eqn (11.29)), the second term in (11.26) is negligible so that one can approximate the Gross-Pitaevskii eqn (11.26) with the new equation −

2 d2 Ψ0 + (r − R)F Ψ0 + gΨ30 = 0. 2m dr2

(11.28)

Let us now introduce the dimensionless variable s = (r − R)/d, where d=

2m F 2

−1/3

=

a4ho 2R

1/3 (11.29)

Finite-size corrections to the Thomas–Fermi limit

177

2 is the characteristic thickness of the boundary and we have used F = mωho R. In terms of the dimensionless function Φ, deﬁned by

Ψ0 (r) =

2 Φ(s), 2mgd2

(11.30)

the Gross-Pitaevskii eqn (11.28) takes the universal form Φ − (s + Φ2 )Φ = 0,

(11.31)

where the nonlinear term Φ3 originates from the nonlinear interaction term of the Gross-Pitaevskii equation. When s → +∞, the solution of (11.31) tends to zero and the cubic term can be neglected. In this limit eqn (11.31) takes the simpler form Φ − sΦ = 0, which deﬁnes the Airy function. The asymptotic behaviour then has the form A 2 2/3 Φ(s → ∞) 1/4 exp − s , 3 2s

(11.32)

where the value of A can be determined by numerical integration of (11.31) (Dalfovo et al., 1996). The coeﬃcient A √ has been calculated analytically by Margetis (2000), who obtained the result A = 1/ 2. In the opposite limit s → −∞ one can neglect the √ second derivative Φ and the asymptotic behaviour is given by Φ(s → −∞) = −s, corresponding to Ψ0 (r) = 2 R/g. The same behaviour is also derivable from the Thomas–Fermi (R − r)mωho result (11.7) in the limit (R − r) R. The full behaviour of the function Φ(s) is shown in Figure 11.4. Results of the numerical solution of the GP equation for all values of r are presented in Figure 11.5. The solution of eqn (11.31) provides, via eqns (11.29) and (11.30), the proper structure of the wave function of the condensate near the classical turning point R. It is worth pointing out that eqn (11.31) does not depend on the form of the external potential, nor on the size of the interatomic force. These physical parameters enter the expression for the reduced variable s and the transformation (11.30) for the wave function of the order parameter. The Thomas–Fermi solution (11.7) and the wave function (11.30) determine the behaviour of the wave function in two distinct regions of space: the former in the interior of the cloud; the latter in the boundary region. For suﬃciently large N these two regions are suﬃciently extended to match each other and hence the solution of the Gross-Pitaevskii equation is deﬁned in a complete way. An example is shown in Figure 11.4. A third region is the one at large distances beyond the boundary. The asymptotic behaviour in this region is determined by the chemical potential. The contribution of this asymptotic region to the relevant energy integrals can, however, be neglected in the Thomas–Fermi regime.

178

Ground State of a Trapped Condensate

φ

2

1

0 −4

−2

0 s

2

4

Figure 11.4 Solution of the universal eqn (11.31). The two asymptotic limits line) and (11.32) (dashed line) are also shown.

√ −s (dot–dash

0.06 N = 105

ψ

0.04

0.02

0

0

2

4 r/aho

6

8

Figure 11.5 Condensate wave function for 105 atoms of 87 Rb (scattering length a = 5.29 × 10−7 cm). Solid line—numerical solution of the GP eqn (11.1); dot–dash line—Thomas–Fermi approximation (11.7) (indistinguishable from the solid line in the inner part); dashed line— surface proﬁle obtained from the universal eqn (11.31).

Finite-size corrections to the Thomas–Fermi limit

179

Let us now apply the above results to the calculation of the kinetic energy. The integral (11.20) can be naturally divided into two parts: +∞ R− 4π2 Ekin = |Ψ (r)|2 r 2 dr + |Ψ (r)|2 r 2 dr , (11.33) 2m 0 R− where the distance > 0 from the boundary R is chosen in order to satisfy the conditions d R.

(11.34)

This permits us to evaluate the ﬁrst term using the Thomas–Fermi approximation (11.7) and the second one using the solution (11.30) of the universal eqn (11.31). The sum of the two terms should not depend on . The ﬁrst integral is easily evaluated and becomes

R− 2R 8 R3 2 2 ln − , (11.35) |Ψ (r)| r dr = 16πa4ho a 3 0 where we have neglected corrections vanishing as /R. The relevant range of integration for the second integral is the boundary region, where the universal eqn (11.31) holds. To the leading order one ﬁnds: +∞ +∞ R3 |Ψ (r)|2 r 2 dr = (φ )2 ds, (11.36) 4πa4ho a −/d R− where φ = dφ/ds. If the ratio /d is suﬃciently large (see condition (11.34)) the integral √ on the right-hand sideis calculated by partial integration. Using the relationship d ln( 1 + s2 + s)/ds = 1/ 1 + s2 ) we can write

+∞

−/d

(φ )2 ds =

1 2 ln + C, 4 d

(11.37)

with C=−

+∞

ln −∞

d (φ )2 1 + s2 ds = 0.176. 1 + s2 + s ds

(11.38)

Collecting the above results and using expression (11.29) for the thickness of the boundary, one ﬁnally ﬁnds the following result for the asymptotic value of the kinetic energy

Ekin 5 2 R 5 2 R = ln + (7/4) ln 2 − 2 + 3C = ln , (11.39) N 2 mR2 aho 2 mR2 1.3aho where we have used the Thomas–Fermi expression N = R5 /(15aa4ho ). Equation (11.39) provides the correct asymptotic behaviour of the kinetic energy in the Thomas–Fermi

180

Ground State of a Trapped Condensate

limit N a/aho 1 or, equivalently, R aho . Notice that the ratio Ekin /N μT F , which ﬁxes the importance of the corrections to the Thomas–Fermi limit, is given by a 4 Ekin R ho =5 ln 0 N μT F R 1.3aho

(11.40)

and vanishes like N −4/5 ln N for large N . Analogous expansions can be derived for the other energy components (oscillator and interaction energies). The corresponding corrections to the Thomas–Fermi limit are determined by the changes in the order parameter with respect to the Thomas– Fermi result (11.7) due to the quantum pressure term in the Gross-Pitaevskii equation. Using the virial theorem (11.24), equation (11.23) for the chemical potential, and the thermodynamic relationship μ = dE/dN it is easy to derive the expression for the energy, analogous to (11.39). One ﬁnds:

E ET F Ekin 5 R 5 2 1 = + = μ0T F + . ln + N N N 7 2 mR2 1.3aho 4

(11.41)

The separate expansions for the oscillator and interaction energies are instead given by

3 R 2 3 Eho = μ0T F + ln + N 7 mR2 1.3aho 8

(11.42)

Eint 2 0 R 2 1 = μT F − ln − , N 7 mR2 1.3aho 4

(11.43)

and

while for the chemical potential (11.23) we obtain the result μ0 = μ0T F +

R 3 2 7 ln + 2 mR2 1.3aho 12

(11.44)

(see Fetter and Feder, 1998 and Zambelli and Stringari, 2002). In the above equations the radius R is given by the Thomas–Fermi expression (11.15). Notice that in the sum Eho + Eint the main logarithmic correction cancels out because this quantity is minimized by the Thomas–Fermi proﬁle (11.7).

11.5

Beyond-mean-ﬁeld corrections

So far we have investigated the ground state of a Bose–Einstein condensate in the framework of mean-ﬁeld GP theory. This approach corresponds to the ﬁrst approximation of Bogoliubov theory for uniform gases. A natural problem concerns the inclusion of higher-order corrections, accounting for the changes in the equation of state due to the occurrence of quantum correlations. In eqn (4.34) we have derived the ﬁrst

Beyond-mean-ﬁeld corrections

181

corrections to the chemical potential of a uniform gas which are determined by the 1/2 gas parameter na3 according to the law 32 3 1/2 . μ(n) = gn 1 + √ na 3 π

(11.45)

Let us now calculate the changes in the equilibrium density proﬁle caused by the new equation of state. If the density is suﬃciently smooth, one can apply the local density approximation to the chemical potential. This yields, at equilibrium, the result μ(n(r)) + Vext (r) = μT F ,

(11.46)

where μ(n) is the chemical potential of the uniform gas evaluated at the density n, while the value of μT F is ﬁxed by the normalization condition for the density and diﬀers from the zeroth order result (eqn (11.8)) because of the presence of beyond-mean-ﬁeld eﬀects. Equation (11.46) can be solved by iteration by treating the correction of (11.45) as a small perturbation. One ﬁnds the result (Timmermans et al., 1997): n(r)T F = n0T F (r) − α(n0T F )3/2 (r),

(11.47)

where n0T F (r) = (μT F − Vext (r))/g is the zeroth order Thomas–Fermi proﬁle (11.7) for the ground state density calculated with a renormalized value of the chemical potential √ to account for the proper normalization of the density, and α = (32/3 π)a3/2 . The new value of the chemical potential is given by √ μT F = μ0T F 1 + π a3 n(0) , (11.48) where μ0T F is the mean-ﬁeld value (11.8) and a3 n(0) =

152/5 8π

12/5 a N 1/6 aho

(11.49)

is the gas parameter evaluated in the centre of the trap (n(0) = μ0T F /g). Beyond-meanﬁeld eﬀects are also responsible for an increase of the Thomas–Fermi radii where the density (11.47) vanishes. In fact, the radii are directly related to the chemical potential by the general TF relation 2μT F = mωx2 R2x = ωy2 Ry2 = ωz2 Rz2 . For suﬃciently large N the beyond-mean-ﬁeld eﬀect turns out to be larger than the correction due to ﬁnite size eﬀects (see eqn (11.44)). This is important in view of the experimental possibility (Navon et al., 2011) of determining the equation of state of uniform matter, starting from the measurement of the density proﬁles (see Section 13.6 and Figure 4.2). At this level of accuracy the density proﬁle (11.47) can no longer be identiﬁed with the condensate density n0 for which, applying the local density approximation to the Bogoliubov result (4.48), one ﬁnds the expression 5 n0 (r) = n0T F (r) − α(n0T F )3/2 (r). 4

(11.50)

182

Ground State of a Trapped Condensate

By integrating eqn (11.50) one ﬁnds the result √ δN0 5 π 3 = a n(0) N 8

(11.51)

for the quantum depletion of the condensate of an atomic gas conﬁned in a harmonic trap. Both results (11.48) for the chemical potential and (11.51) for the quantum depletion are similar to the expansions (4.34) and (4.48), which hold in uniform matter.

11.6

Attractive forces

If the interatomic forces are attractive (a < 0), the behaviour of the solutions of the Gross-Pitaevskii equation is quite diﬀerent. In this case the gas tends to increase its density in the centre of the trap in order to lower the interaction energy. This tendency is contrasted by the zero-point kinetic energy which can stabilize the system. However, if the central density grows too much, the kinetic energy is no longer able to avoid the collapse of the gas. The collapse is expected to occur when the number of particles in the condensate exceeds a critical value Ncr , of the order of aho /|a|. It is worth stressing that in a uniform gas, where quantum pressure is absent, the condensate is always unstable, so that the existence of metastable conﬁgurations with negative scattering length is a remarkable feature produced by the external trapping. The critical number Ncr can be calculated at zero temperature by means of the Gross-Pitaevskii equation. The solutions of this equation for negative a correspond to local minima of the energy functional (11.19). When N increases, the depth of the local minimum decreases. Above Ncr the minimum no longer exists and the Gross-Pitaevskii equation has no solution. For a spherical trap this happens at (Ruprecht et al., 1995) Ncr |a| = 0.575. aho

(11.52)

A physical insight into the behaviour of the gas with attractive forces can be obtained by means of a variational approach based on Gaussian functions. For a spherical trap one can minimize the energy (11.19) using the ansatz φ(r) =

N w3 a3ho π 3/2

1/2

exp −

r2 , 2w2 a2ho

(11.53)

where w is a dimensionless variational parameter which ﬁxes the width of the condensate. One obtains 3 E(w) N |a| −3 = (w−2 + w2 ) − (2π)−1/2 w . Nωho 4 aho

(11.54)

This energy is plotted in Figure 11.6 as a function of w for several values of the parameter N |a|/aho . One clearly sees that the local minimum disappears when this

Attractive forces

183

5

4

0.3

3 E/N

0.4

2

0.5 0.6

1 0.7

0

0

0.5

1 w

1.5

2

Figure 11.6 Energy per particle, in units of ωho , for atoms in a spherical trap with attractive forces, as a function of the eﬀective width w in the Gaussian model of eqns (11.53) and (11.54). Curves are plotted for several values of the parameter N |a|/aho . In the Gaussian model the minimum disappears for N |a|/aho = 0.671.

parameter exceeds a critical value. This can be calculated by requiring that the ﬁrst and second derivative of E(w) vanish at the critical point (w = wcr and N = Ncr ). One ﬁnds wcr = 5−1/4 ≈ 0.669 and Ncr |a|/aho ≈ 0.671. The last formula provides an estimate of the critical number of atoms, reasonably close to the value (11.52) obtained by solving exactly the GP equation. Experiments with trapped Bose gases interacting with negative scattering length were ﬁrst carried out with lithium vapours (Bradley et al., 1995 and 1997). The measurements are consistent with the theoretical predictions for the maximum number of atoms that can be hosted in the condensate. More recently, it has been possible to carry out experiments on 85 Rb condensates, where the value of the scattering length was tuned by applying an additional magnetic ﬁeld (Roberts et al., 2001). These experiments have permitted the exploration, in a quantitative way, of the dependence of the critical number on the value of the scattering length. The results seem to suggest that condensates collapse at a slightly lower value of the interaction strength than predicted by GP theory. For an accurate comparison with theory one should also take into account the role of the deformation of the trap.

12 Dynamics of a Trapped Condensate The study of elementary excitations is a subject of primary importance in the physics of quantum many-body systems. In superﬂuid helium it was the subject of pioneering theoretical work by Landau, Bogoliubov, and Feynman. After the experimental realization of Bose–Einstein condensation in trapped atomic gases, the study of collective excitations has also become a popular subject of research in ultracold gases. From the theoretical side new challenging features emerge because of the nonuniform nature of these systems (Sections 12.1–12.5). From the experimental side the measurement of the collective frequencies can be carried out with high precision, therefore providing a unique opportunity for detailed comparison with theory. We will also consider the case of the large-amplitude oscillations (Section 12.6), where interesting phenomena are predicted in the presence of degeneracy between the frequencies of the collective oscillation and the second harmonics of lower-frequency modes. The importance of this nonlinear coupling can be tuned by changing the deformation of the trap. Another important problem is the expansion of the condensate after the sudden switching oﬀ of the conﬁning trap (Section 12.7). This problem is particularly relevant because most measurements on Bose–Einstein condensates are actually taken after expansion. We will then focus on the behaviour of the dynamic structure factor of trapped Bose– Einstein condensates (Section 12.8). We will show how this quantity can be measured and what the key features exhibited by trapped Bose–Einstein condensates are. In particular, the dynamic structure factor permits us to obtain information not only on the collective properties of the system, but also on the particle momentum distribution, a quantity of major interest in the presence of BEC. In the last section we will discuss the role played by single-particle excitations which are predicted to be mainly concentrated in the surface region and contribute in a crucial way to the density of states and consequently to the thermodynamic behaviour of the trapped BEC.

12.1

Collective oscillations

The theory of elementary excitations for nonuniform Bose condensates at zero temperature has been reviewed in Chapter 5, to which we refer for the development of the formalism. The collective oscillations are described by the linearized solutions of the time-dependent Gross-Pitaevskii equation

i

∂ Ψ(r, t) = ∂t

2 2 ∇ − + Vext (r, t) + g|Ψ(r, t)|2 Ψ(r, t), 2m

(12.1)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Collective oscillations

185

and hence correspond to the classical oscillations of the order parameter in the limit of small amplitudes. By writing the order parameter in the form Ψ(r, t) = Ψ0 (r,t) exp(−iμt/) = exp(−iμt/) (Ψ0 (r) + ui (r) exp(−iωt) + vi∗ (r) exp(iωt)) one derives the coupled equations (5.69), namely 2 2 ∇ + Vext − μ + 2gn0 (r) ui (r) + g(Ψ0 (r))2 vi (r), − 2m 2 2 ∇ + Vext − μ + 2gn0 (r) vi (r) + g(Ψ∗0 (r))2 ui (r) (12.2) −ωi vi (r) = − 2m ωi ui (r) =

for the Bogoliubov quasi-particle amplitudes ui and vi . In these equations n0 = |Ψ0 (r)|2 is the ground state solution of the stationary Gross-Pitaevskii equation (11.1). The solutions of eqn (12.2) provide the frequencies ωi of the elementary excitations of the system. In this chapter the trapping potential will be assumed to have the harmonic form Vext (r) =

1 1 1 mωx2 x2 + mωy2 y 2 + mωz2 z 2 . 2 2 2

(12.3)

In contrast to a uniform system, where the solutions of (12.2) give rise to the famous Bogoliubov dispersion law (4.31), in the presence of nonuniform conﬁnement momentum is not a good quantum number and consequently the elementary excitations should be classiﬁed taking into account the new symmetries of the problem. For spherical trapping angular momentum and its third component m are the natural quantum numbers. In most experimental situations the trapping is, however, only axisymmetric. In this case m is still a good number, but diﬀerent values of are coupled by the external potential. In Figure 12.1 we show the results for the collective frequencies with m = 0 and m = 2 obtained by solving numerically the Bogoliubov equations (12.2) for the lowest modes of even multipolarity for a gas of rubidium atoms conﬁned in a disc-shaped trap (ω⊥ < ωz ) (Edwards et al., 1996; see also Esry, 1997 and You et al., 1997)). In the limit of spherical trapping these modes coincide with the lowest monopole ( = 0) and quadrupole ( = 2) excitations, respectively. The interesting feature emerging from both the experimental (Jin et al., 1996) and theoretical results is the deviation from the prediction of the noninteracting model which, for these modes, would be ω = 2ω⊥ . The deviations become more and more visible as N increases. In the large N limit the theoretical curves approach an asymptotic value that will be discussed in the following section. Among the various oscillations exhibited by these trapped gases, special attention should be devoted to the dipole mode. This oscillation corresponds to the motion of the centre of mass of the system, which, due to the harmonic conﬁnement, oscillates with the frequency of the harmonic trap (this frequency can of course be diﬀerent in the three directions). Two-body interactions cannot aﬀect this mode because the motion of the centre of mass is exactly decoupled from the internal degrees of freedom of

186

Dynamics of a Trapped Condensate 2 m=0

Frequency

1.8

1.6 m=2

1.4

1.2

0

0.5

1

1.5

Na/aho

Figure 12.1 Frequency (in units of ω⊥ ) of the lowest collective modes of even parity, m = 0 √ and m = 2, for N rubidium atoms in the JILA trap (λ = 8). Points are the experimental results of Jin et al. (1996). Solid lines are the predictions of the mean ﬁeld eqns (12.2). Dashed lines are the asymptotic results in the Thomas–Fermi limit (Stringari, 1996b). Here one has a/a⊥ = 3.37 × 10−3 .

the system. This is best understood by considering the time-dependent equation (12.1) and looking for solutions of the form Ψ0 (r, t) = e−iφ(t)/ eizβ(t)/ Ψ0 (x, y, z − α(t)),

(12.4)

where Ψ0 (r) is the equilibrium solution and, for simplicity, we have considered an oscillation along the z-axis. By a proper change of the variable z → z − α, one ﬁnds that (12.4) is an exact solution of the time-dependent Gross-Pitaevskii equation, ˙ The solution then corresponds to a harmonic provided β = mα˙ and αmωz2 = −β. oscillation of frequency ωz , holding also for large amplitudes. The occurrence of this mode characterizes any system conﬁned by a harmonic potential, at zero as well as ﬁnite temperatures, and is independent of interactions and quantum statistics. This remarkable property was originally proven by Kohn (1961) in the context of the cyclotron frequency of electrons in metals and is known as Kohn theorem. The fact that the dipole frequency is not aﬀected by two-body interactions provides a direct test on the numerical accuracy of the various methods used to solve the equations of motion. On the other hand, its experimental measurement turns out to be a very useful procedure

Repulsive forces and the Thomas–Fermi limit

187

for checking the harmonicity of the trap and for determining with high accuracy the value of the trapping frequencies.

12.2

Repulsive forces and the Thomas–Fermi limit

When the number of atoms in the trap increases the eigenfrequencies of the Bogoliubov eqns (12.2), for a ﬁxed choice of the quantum numbers, approach an asymptotic value, which is achieved when the Thomas–Fermi condition N a/aho 1 is satisﬁed. In this limit one can neglect the quantum pressure term and the motion is properly described by the hydrodynamic theory of superﬂuids. In Section 5.2 we have derived the corresponding equations, which take the form ∂n + div(vn) = 0 ∂t

(12.5)

and ∂ m v+∇ ∂t

1 mv2 + Vext + μ(n) 2

= 0,

(12.6)

where μ(n) = gn. In these equations the density and the velocity ﬁeld are related to the order parameter Ψ(r, t) = |Ψ(r, t)|eiS(r,t) through the relationships n(r, t) = |Ψ(r, t)|2

(12.7)

and v(r, t) =

∇S(r, t). m

(12.8)

It can immediately be seen that the stationary solution of eqn (12.6) coincides with the Thomas–Fermi density proﬁle (11.7). Conversely, the time-dependent equations, after linearization, take the simpliﬁed form

! ∂2 ∂μ δn = ∇ · c2 (r)∇δn , δn = ∇ · n(r)∇ (12.9) ∂t2 ∂n where δn(r, t) = n−n(r) is the change of the density proﬁle with respect to the equilibrium conﬁguration n(r) and mc2 (r) = gn(r) = (μT F − Vext (r)). In deriving the second equality of (12.9) we have made explicit use of the linear dependence of the chemical potential on the density of the BEC gas. The quantity c(r) has the clear meaning of a local sound velocity. The validity of eqns (12.6) and (12.9) is based on the assumption that the spatial variations of the density are smooth not only in the ground state, but also during the oscillation. In a uniform system (Vext ≡ 0) this is equivalent to requiring that the collective frequencies are much smaller than the chemical potential or, equivalently, that the wavelength is much larger than the healing length (5.20). In the uniform case thesolutions of (12.9) are sound waves propagating with the Bogoliubov velocity c = gn/m. Sound waves can also propagate in nonuniform media,

188

Dynamics of a Trapped Condensate

Speed of sound [mm/s]

provided we look for solutions varying rapidly with respect to the size of the system, so that one can assume a locally uniform sound velocity. In conclusion, the conditions required to have sound waves in trapped condensates are that qL 1 and qξ 1 are satisﬁed, where L is the size of the condensate, q is the wave vector of the sound wave, and ξ is the healing length. Furthermore, if the system is highly deformed and cigar-shaped, one can simultaneously satisfy the conditions qZ 1 and qR⊥ 1, characterizing the propagation of one-dimensional waves along z. Here Z and R⊥ are the radii of the condensate in the axial and radial directions, respectively. In this case one region of the trap is given by can show that the sound velocity in the central μ/2m, instead of the usual Bogoliubov value μ/m (Zaremba, 1998). The reduction of the sound velocity with respect to the central value follows from the fact that in this ‘one-dimensional’ geometry, the sound velocity is ﬁxed by the density averaged over the radial direction, which is of course smaller than its central value (see also Section 24.1). Experimentally sound waves in Bose–Einstein condensed gases can be generated by focusing a laser pulse in the centre of a cigar-type trap. A wave packet forms in this way, propagating outwards, which can be imaged at diﬀerent times so that the value of the sound velocity can be directly measured. In Figure 12.2 we show the observed values of c at diﬀerent densities. The agreement with the theoretical prediction μ/2m = gn(0)/2m, where n(0) is the value of the density in the centre of the trap, is reasonably good, especially at high density. In addition to the propagation of wave packets, characterized by wavelengths much shorter than the size of the system, one can look for solutions of eqn (12.9)

10

5

0 0

2

4 Density [1014 cm–3]

6

8

Figure 12.2 Speed of sound c versus condensate peak density n(0) for waves propagating along the axial direction in the cigar-shaped condensate at MIT. The experimental points are compared with the theoretical prediction c = gn(0)/2m (solid line). From Andrews et al. (1997a). Source: Reprinted with permission from Physical Review Letters, 79, 553; c 1997, American Physical Society.

Repulsive forces and the Thomas–Fermi limit

189

corresponding to a motion involving the whole condensate. These solutions have frequencies of the order of the oscillation frequencies and correspond to the lowfrequency modes discussed in the previous section. They can be worked out in an analytic way starting from the linear hydrodynamic eqn (12.9). For a spherical trap the solutions are deﬁned in the interval 0 < r < R and have the form (2n ) (2n) δn(r) = P r (r/R) r Ym (θ, φ), where P are polynomials of degree 2n, containing only even powers. The quantum number nr provides the number of nodes of the radial wave function. By inserting the above ansatz for δn(r) into eqn (12.9) one obtains the result (Stringari, 1996b) ω(nr , ) = ωho (2n2r + 2nr + 3nr + )1/2

(12.10)

for the dispersion law of the discretized normal modes. This result should be compared with the prediction of the ideal gas model in a harmonic potential: ω(nr , ) = ωho (2nr + l),

(12.11)

with 2nr + l = nx + ny + nz (see eqn (10.4)). Of particular interest is the case of the so-called √ surface excitations (nr = 0) for which eqn (12.10) predicts the dispersion law ω = ωho . The frequency of these modes is systematically smaller than the result ωho holding in the ideal gas model. Notice that in the dipole case (nr = 0, = 1) the prediction (12.10) coincides with the oscillator frequency, in agreement with the general considerations about the centre-of-mass motion discussed in the previous section. For the compressional modes (nr = 0), the lowest solution of (12.9) is the monopole oscillation, also called the breathing mode, characterized √ by the quantum numbers nr = 1 and = 0. The formula (12.10) gives the result 5 ωho which is higher than the prediction 2ωho of the noninteracting model. For a ﬁxed value of N the accuracy of prediction (12.10) is expected to become lower and lower as nr and increase. In fact, for large nr and the oscillations of the density have shorter wavelength and neglecting the quantum pressure term in the GrossPitaevskii equation is no longer justiﬁed. In analogy with the case of uniform Bose gases, the condition for the applicability of the hydrodynamic theory of superﬂuids is expected to be ω < μ. However, more severe restrictions are imposed when one considers single-particle excitations localized near the boundary of the condensate (see Section 12.9). Result (12.10) reveals that, in the Thomas–Fermi limit N a/aho 1, the dispersion relation of the normal modes of the condensate has changed signiﬁcantly from the noninteracting behaviour (12.11). However, at ﬁrst sight it is surprising that in this limit the dispersion does not depend on the value of the interaction parameter a. This diﬀers from the uniform case where the dispersion law, in the corresponding phonon regime, is given by ω = cq and depends explicitly on the interaction through the velocity of sound. The behaviour exhibited in the harmonic trap is well understood if one notes that the discretized values of q are ﬁxed by the boundary and vary as /R, where R is the size of the system. While in the box this size is ﬁxed, in the

190

Dynamics of a Trapped Condensate

case of harmonic conﬁnement it increases with N due to the repulsive eﬀect of twobody interactions (see eqn (11.14)): R ∼ (N a/aho )1/5 (/mωho )1/2 . On the other hand, the velocity, calculated at the centre of the trap, is given by c = value of the sound μ/m = (N a/aho )1/5 (ωho /m)1/2 and also increases with N . When one takes the product cq both the interaction parameter and the number of atoms in the trap cancel out, so that the frequency turns out to be proportional to the bare oscillator frequency ωho . A similar argument holds for the surface excitations. In fact, in the presence of an external force the dispersion relation of the surface modes obeys the classical law ω 2 = qF/m, where the force F should be evaluated at the surface of the system. In our case, using the linear ramp expansion for the external potential (see Section 11.5), we 2 have F = mωho R, where R is the radius of the condensate. Since the product qR gives (in units of ) the angular momentum carried by the wave, one recovers the dispersion √ law ωho of the surface excitations. The results for the elementary excitations in the presence of a spherical trap can be generalized to include anisotropic conﬁgurations. Let us consider the case of a harmonic oscillator potential with axial symmetry along the z axis. In this case the diﬀerential equation (12.9) takes the form m

' & ∂2 m 2 2 2 2 ω ∇δn , δn = ∇ · μ − r + ω z 0 ⊥ ⊥ z ∂t2 2

(12.12)

where we have used mc2 (r) = μ0 − Vext (r). Because of the axial symmetry of the trap the third component m of the angular momentum is still a good quantum number. However, the dispersion law now depends on m. Explicit results are available in some particular cases. For example, quadrupole solutions of the form δn = r 2 Y2m (θ, φ) still satisfy the hydrodynamic eqn (12.12) for m = ±2 and m = ±1. The resulting dispersion laws are: 2 ω 2 ( = 2, m = ±2) = 2ω⊥

(12.13)

2 + ωz2 . ω 2 ( = 2, m = ±1) = ω⊥

(12.14)

and

Conversely, the = 2, m = 0 mode is coupled to the monopole = 0 excitation and the dispersion law of the two decoupled modes is given by 3 1 2 ω 2 (m = 0) = 2ω⊥ + ωz2 ∓ 2 2

#

2 4 9ωz4 − 16ωz2 ω⊥ + 16ω⊥ .

(12.15)

√ When ωz =√ ω⊥ ≡ ωho one recovers the solutions for the quadrupole ( 2ωho ) and monopole ( 5ωho ) excitations in the spherical trap. The above results can be generalized to a triaxially deformed potential of the form Vext = (1/2m)(ωx2 y 2 + ωy2 y 2 + ωz2 z 2 ). In this case the six modes described by eqns (12.13)–(12.15) are coupled

Repulsive forces and the Thomas–Fermi limit

191

with each other. The decoupled oscillations consist of three solutions of the form δn = ax2 + by 2 + cz 2 whose eigenfrequencies obey the equation ω 6 − 3ω 4 (ωx2 + ωy2 + ωz2 ) + 8ω 2 (ωx2 ωy2 + ωy2 ωz2 + ωz2 ωx2 ) − 20ωz2 ωy2 ωz2 = 0,

(12.16)

and three solutions of the form δn = αxy, βyz, and γxz with frequencies ω 2 = ωx2 +ωy2 , ωy2 + ωz2 , and ωx2 + ωz2 , respectively. In the case of deformed condensates the latter solutions correspond to the so-called scissors mode, i.e. to the oscillating rotation of the atomic cloud in the xy, yz, and xz planes, respectively. The scissors mode characterizes the rotational properties of the condensate and will be discussed in more detail in Chapter 14. From Figure 12.1 one can see that the JILA experiments for the m = 0 and m = 2 modes do not fully fall into the Thomas–Fermi regime described by eqns (12.13)–(12.15). Conversely, the experimental results obtained on sodium vapours at MIT in 1998 (Stamper-Kurn et al., 1998c), see Figure 12.3, represent a beautiful example of excitations belonging to the Thomas–Fermi regime. In this experiment the magnetic trap has an axisymmetric cigar shape with ωz ω⊥ . Furthermore, the number of atoms is very high, so that the condition N a/aho 1 is well satisﬁed and the energies of the collective oscillations along the axial direction are much smaller than the chemical potential. This explains the excellent agreement between the observed frequency ω/ωz = 1.569(4) for the lowest axial m = 0 mode of even parity and the theoretical prediction ω/ωz = 5/2 = 1.581 given by the lowest solution of eqn (12.15) in the limit ωz ω⊥ . In the same limit ωz ω⊥ the highest solution approaches the value 2ω⊥ . The coincidence of this result with the ideal gas prediction for the same mode is not accidental. Actually, one can prove on a very general basis that the radial m = 0 oscillation of a very elongated condensate has frequency 2ω⊥ , and is independent of the interaction

350 μm

5 milliseconds per frame

Figure 12.3 Collective oscillation of a Bose–Einstein condensate. In situ repeated phasecontrast images of a ‘pure’ condensate are shown. Both the centre of mass and the shape oscillations are visible. The ﬁeld view in the vertical direction is about 620 μm. The time step is 5 ms per frame. From Stamper-Kurn and Ketterle (1998).

192

Dynamics of a Trapped Condensate

as well as of the amplitude of the oscillation (Pitaevskii, 1996; Kagan et al., 1996). To prove this interesting behaviour let us the time-dependent equation for the derive 2 2 average radial square radius r⊥ = 1/N drr⊥ n(r, t). From the equation of continuity one immediately ﬁnds the result d 2 2 r⊥ = dt N

drr⊥ · j(r, t),

(12.17)

where j(r, t) is the current density (5.10). By taking the time derivative of (12.17) and using equations (5.13) and (5.14) for the current density one obtains, after some straightforward algebra, the following equation: 2 d2 2 4 E 2 2 − 2 p2z − 2ωz2 rz2 , r = −4ω⊥ r⊥ + dt2 ⊥ mN m

(12.18)

where E is the total energy of the system (see eqn (5.8)) which is conserved in time, and p2z /2m and mωz2 z 2 are, respectively, the axial contribution to the kinetic and oscillator energies. Result (12.18) is exact within the Gross-Pitaevskii scheme. It is not restricted to the Thomas–Fermi regime, nor to the linear limit. In a highly elongated trap (ωz ω⊥ ) the radial motion couples weakly with the axial degrees of freedom so that one can neglect the time variation of the terms p2z and rz2 in eqn (12.18). 2 The equation for r⊥ is hence also harmonic for large-amplitude oscillations and is characterized by the frequency ω = 2ω⊥ . This behaviour has been checked with high accuracy in the experiment of Chevy et al. (2002), see Figure 12.4, which has further pointed out that this radial oscillation is very weakly damped.

A(t) / A

1.6

1.2

0.8

0.4 0

2

4

6

8 Time [ms]

10

12

14

Figure 12.4 Variation of the radial square radius A(t) = Rx2 (t) + R2y (t) after a strong excitation of the transverse breathing mode in a cigar-shaped condensate. The line is a sinusoidal ﬁt of the data. The ﬁgure shows that this oscillation has a very small damping. From Chevy c 2002, et al. (2002). Reprinted with permission from Physical Review Letters, 88, 250402; American Physical Society.

Sum rule approach: from repulsive to attractive forces

193

For highly deformed traps it is also possible to obtain simple analytic results for the excitations with higher quantum numbers. The resulting expressions will be discussed in Sections 23.1 and 24.1 for pancake and cigar conﬁgurations, respectively. Let us ﬁnally remark that the results for the discretized frequencies derived in this section were derived in the presence of harmonic trapping. They diﬀer signiﬁcantly from the ones derived in the presence of a box potential, where the equilibrium density is uniform inside the trap. For example, in the presence of a cylindrical box potential, the same hydrodynamic equation (12.9) gives the analytic solutions δn ∝ sin(qz) (cos(qz)) for odd (even) oscillations propagating along the symmetry axis of the trap. The corresponding collective frequencies are ω = cq where c is the sound velocity of uniform matter, the value of q being ﬁxed by imposing the boundary condition that the velocity vz ∝ ∂z δn should vanish at the border. This gives the value q = (n − 1/2)π/L and q = nπ/L for the odd and even mode oscillations, respectively, with n = 1, 2 . . . and 2L the length of the cylinder. The lowest mode (n = 1) with odd parity has recently been measured by Navon and Hadzibabic (2015), who found good agreement with the theoretical prediction for samples satisfying the Thomas–Fermi condition ξ L.

12.3

Sum rule approach: from repulsive to attractive forces

A useful insight into the behaviour of the collective excitations can be obtained using the formalism of a linear response function and of sum rules developed in Chapter 7. A major advantage of this method is that the moments mp = (ω)p S(ω)dω of the dynamic structure factor SF (ω) = |0|F |n |2 δ(ω − ωn0 ) (12.19) n

associated with a given excitation operator F can often be evaluated using algebraic techniques, avoiding the full solution of the equations of motion. For example, the energy-weighted moment takes the simple form (in this section we consider Hermitian operators) m1 =

1 0|[F, [H, F ]]|0. 2

(12.20)

Furthermore, if the operator F depends only on the spatial coordinates, only the kinetic energy term in the Hamiltonian contributes to m1 , whose calculation becomes straigthtforward. Choosing for F the dipole operator (F = i zi ) one ﬁnds the model independent result m1 = N2 /2m, analogue of the Thomas–Reich– Kuhn sum results are also obtained for the monopole 2rule of atomic physics. Simple 2 2 (F = r ) and quadrupole (F = (3z i i − ri )) operators, for which we ﬁnd the i i 2 2 2 2 results m1 = 2N r /m and m1 = 4N x + y 2 + 4z 2 /m, respectively. In a similar way one may also obtain compact results for the cubic energy-weighted moment, which can be written in the form m3 =

1 0|[[F, H], [H, [H, F ]]]|0. 2

(12.21)

194

Dynamics of a Trapped Condensate

Unlike m1 and m3 , the inverse energy-weighted moment m−1 cannot easily be calculated in terms of commutators. Formally, one can always write m−1 = 0|[F, X]|0/2, where the operator X is deﬁned by the commutation rule [H, X] = F . However, except in special cases, this equation cannot be solved algebraically. The sum rule m−1 is however related to the static response χ (compressibility sum rule, see eqn (7.24)) which in some cases can be evaluated directly. Let us consider the monopole F = i ri2 excitation (breathing mode). In this case the polarizability χM is ﬁxed by the linear change δr 2 = λχM of the mean square radius induced by the static perturbation −λF . Adding this ﬁeld to the Hamiltonian is equivalent to renormalizing the trapping harmonic potential and for isotropic conﬁnement one can simply write χM = −

2N ∂r 2 2 , m ∂ωho

(12.22)

where ωho is the frequency of the harmonic oscillator. Using the scaling properties of the Gross-Pitaevskii equation (11.10), one can exactly express the derivative 2 ∂r2 /∂ωho in terms of the square radius r2 , and its derivative with respect to N . A straightforward calculation yields (Zambelli and Stringari, 2002)

N N ∂ 2 2 χM = r r − . (12.23) 2 mωho 2 ∂N Using the moments m1 and m−1 one can deﬁne an average excitation energy through the ratio (ω)2 =

m1 r 2 = −2 2 , m−1 ∂r 2 /∂ωho

(12.24)

yielding the useful result 2 2 ωM = 4ωho

r 2

r2 . − (N/2)∂r2 /∂N

(12.25)

for the frequency of the breathing mode. In the noninteracting case, the square radius is independent of N and one recovers the result ωM = 2ωho . Conversely, in the Thomas–Fermi limit, where N a/aho is large and positive, √ the square radius behaves like N 2/5 and eqn (12.25) provides the result ωM = 5 ωho , already derived in the previous section starting from the hydrodynamic equations. It is worth noticing that result (12.25) can also be used to investigate condensates interacting with attractive forces. In this case the square radius decreases with N and the frequency of the breathing mode becomes smaller and smaller. For negative a and close to the critical size Ncr characterizing the onset of instability, the monopole frequency tends to zero because the compressibility of the system becomes larger and larger (Figure 12.5). The comparison with the numerical solutions of the Bogoliubov equations (12.2) (circles) shows that the sum rule estimate (12.25), which in general provides an upper bound to the lowest monopole energy, gives an excellent approximation to the collective frequency

Sum rule approach: from repulsive to attractive forces

195

2.5

Frequency

ωM 2 ωQ 1.5

1 −1

0

1

2

N a/aho

Figure 12.5 Frequencies of the monopole and quadrupole excitations of a condensate in a spherical trap as a function of the parameter N a/aho , for positive and negative values of a. The solid line for the monopole mode is obtained from the ratio (m1 /m−1 )1/2 , as in eqn (12.25). For the quadrupole mode it corresponds to the ratio (m3 /m1 )1/2 , as in eqn (12.27). Solid and empty circles are the eigenenergies of the linearized time-dependent GP eqns (12.2).

for both positive and negative values of a. According to the discussions of Chapter 7, this agreement reveals that the strength distribution of the monopole operator F is almost close to a δ function located at the energy of the lowest compressional mode. This behaviour is also proven by the calculation of the ratio (ω)2 = m3 /m1 for which, assuming isotropic trapping, one ﬁnds the result (Stringari, 1996b) Ekin 2Ekin + 6Eho + 6Eint 2 (ωM ) = = ωho 5 − , N mr 2 Eho 2

(12.26)

where, in the second equality, we have used the virial identity (11.24) to express the mean-ﬁeld interaction energy Eint in terms of the mean-ﬁeld kinetic energy Ekin . The numerical calculation of the monopole frequency, based on eqn (12.26), yields results practically indistinguishable from the ratio m1 /m−1 of eqn (12.25) except near the critical point N = Ncr . Unlike for the monopole, the quadrupole frequency increases with N when a < 0, due to the increase of the kinetic energy of the condensate. This behaviour is well understood by calculating the quadrupole frequency through the ratio m3 /m1 , where m1 and m3 are, respectively, Nthe energy- and cubic energy-weighted moments for the quadrupole operator F = i=1 (3zi2 − ri2 ). By explicitly working out the commutators of the two sum rules one ﬁnds the useful result (Stringari, 1996b) Ekin 2 2 = 2ωho ωQ 1+ . Eho

(12.27)

196

Dynamics of a Trapped Condensate

In the noninteracting gas one has Ekin = Eho and (12.27) gives the harmonic oscillator result ωQ = 2ωho . In the Thomas–Fermi√limit N a/aho 1, the kinetic energy term is negligible and one ﬁnds the value ωQ = 2 ωho , while for negative a the kinetic energy term is larger than Eho and one ﬁnds an enhancement of the quadrupole frequency. The numerical results are reported in Figure 12.5, where one can also see that in the quadrupole case the sum rule estimate is very close to the exact result obtained by numerically solving the Bogoliubov equations. It is ﬁnally worth pointing out that the sum rule method also permits us to evaluate in a straightforward way the frequency associated with the centre-of-mass oscillation. In fact, the commutator [H, k zk ] = −(i/m) k pzk is proportional to the z-component of the total momentum of the system, a quantity which commutes both with the kinetic energy operator and with the two-body potential due to translational invariance. The sum rule m3 is hence determined by the harmonic oscillator potential and exactly yields, for the ratio m3 /m1 , the oscillator energy ωz .

12.4

Finite-size corrections to the Thomas–Fermi limit

The sum rule approach can be usefully employed to determine the ﬁrst correction to the hydrodynamic results discussed in Section 12.2 due to ﬁnite-size eﬀects. Using the expansion (11.42) for Eho the asymptotic behaviour of the monopole frequency (12.26), based on the ratio m3 /m1 , becomes (Zambelli and Stringari, 2002) √ 7 Ekin , (12.28) ωM = 5ωho 1 − 30 N μ where the perturbative correction Ekin /N μ is given by (see eqn (11.39)) a 4 R Ekin ho =5 ln N −4/5 ln N. Nμ R 1.3aho

(12.29)

Equation (12.29) shows that, as expected, the ﬁrst correction to the hydrodynamic 2 value 5ωho is negative. Starting from eqn (12.25) and relating the value of r 2 to Eho , one can also expand the ratio m1 /m−1 for large N . Within logarithmic accuracy, the corresponding expansion coincides with eqn (12.28). The same procedure, applied to the quadrupole frequency (12.27), yields the expansion, √ 7 Ekin ωQ = 2ωho 1 + . (12.30) 6 Nμ Equations (12.28) and (12.30) show that the ﬁnite-size corrections to the monopole and quadrupole oscillations have opposite sign, in accordance with the results of Figure 12.5.

12.5

Beyond-mean-ﬁeld corrections

In the preceding sections we have investigated the collective oscillations of a Bose– Einstein condensate in the framework of mean-ﬁeld GP theory. This approach

Beyond-mean-ﬁeld corrections

197

corresponds to the ﬁrst approximation of Bogoliubov theory for uniform gases. A natural problem concerns the inclusion of higher-order corrections, accounting for the changes in the equation of state due to the occurrence of quantum correlations (see eqn (11.45) and Section 4.2). In order to calculate the consequences of beyond-mean-ﬁeld eﬀects on the frequency of the collective oscillations one can still use the linearized hydrodynamic equation ∂ 2 δn ∂μ m 2 − ∇· n∇ δn = 0, (12.31) ∂t ∂n for the density variations δn(r, t) = n(r, t) − n(r) with respect to equilibrium, by just replacing the expression gn for the chemical potential with the new value (11.45). Using the expansions (11.47) and (11.45) for the ground state density and for the chemical potential, eqn (12.31) takes the form 1 mω 2 δn + ∇· gn0T F ∇δn = − ∇2 αg(n0T F )3/2 δn , (12.32) 2 √ holding at ﬁrst order in the perturbation α = (32/3 π)a3/2 . Equation (12.32) provides the appropriate generalization of the hydrodynamic equation (12.9) derived starting from the GP equation, which is recovered by setting the right-hand side of (12.32) equal to zero. Once the solutions of the hydrodynamic equations derived in the GP regime are known, eqn (12.32) can easily be solved by treating its right-hand side as a small perturbation. One ﬁnds that the corresponding frequency shifts obey the general equation d3 r(∇2 δn∗ )δn(n0T F )3/2 δω αg =− , (12.33) ω 4mω 2 d3 rδn∗ δn where δn and ω are the solutions of the hydrodynamic equations in the GP regime. The integrals of (12.33) extend to the region where the Thomas–Fermi density is positive. Let us ﬁrst remark that the surface modes, satisfying the condition ∇2 δn = 0, are not aﬀected by the change of the equation of state. The lowest compression mode in a spherical trap is the√monopole (breathing) oscillation, characterized by the zerothorder dispersion ω = 5ω0 and by density oscillations of the form δn ∼ (r2 − 3/5R2 ). In this case eqn (12.33) yields the result √ 63 π 3 δωM = a n(0) , (12.34) ωM 128 showing that the fractional shift of the monopole frequency is proportional to the square root of the gas parameter (11.49) evaluated in the centre of the trap. The relative frequency shift (12.34) exhibits the same dependence on the gas parameter as the quantum depletion of the condensate (see eqn (11.51)). Using, for example, N = 106 and a/aho = 6 10−3 , one predicts a relative shift of about 1%. Larger values of δω can be obtained when working near a Feshbach resonance. The above results

198

Dynamics of a Trapped Condensate

were obtained by Pitaevskii and Stringari (1998) and Braaten and Pearson (1999), who also derived the frequency shifts in the presence of deformed traps. It is ﬁnally interesting to compare the above shifts with the ﬁnite-size corrections discussed in the preceding section. For suﬃciently large N one ﬁnds that beyond-mean-ﬁeld eﬀects provide the leading correction to the frequency shift of the compressional modes.

12.6

Large-amplitude oscillations

So far we have discussed the behaviour of the normal modes of the condensate. These correspond to the linearized solutions of the time-dependent Gross-Pitaevskii equation (12.1). It is also interesting to investigate the behaviour of the large-amplitude oscillations. From the theoretical viewpoint one can again attack the problem by starting from the time-dependent Gross-Pitaevskii equation. Indeed, the GP eqn (12.1) for the order parameter of the condensate can be applied to the nonlinear regime, and it is important to check the validity of its predictions through a direct comparison with experiments. When the number of atoms in the trap is large, the time-dependent GP equation (12.1) reduces to the hydrodynamic equations (12.5) and (12.6). The applicability of these equations is not restricted to the linear regime and can be used to investigate nonlinear phenomena in a simpliﬁed way. In general, the frequencies of the trapping potential (12.3) can depend on time, namely ωi = ωi (t). Their static values, ω0i = ωi (0), ﬁx the initial equilibrium conﬁguration of the system, corresponding to the Thomas– Fermi density (11.7). One can easily prove that the hydrodynamic equations admit a class of solutions where the density has the form (Castin and Dum 1996; Kagan et al., 1996; Dalfovo et al., 1997c) y2 z2 x2 n(r, t) = n0 (t) 1 − 2 − 2 − 2 (12.35) Rx (t) Ry (t) Rz (t) within the region where n(r, t) is positive and n(r, t) = 0 elsewhere. The velocity ﬁeld v = (/m)∇S is instead parameterized as v(r, t) =

1 ∇[αx (t)x2 + αy (t)y 2 + αz (t)z 2 ], 2

(12.36)

corresponding to a quadratic ansatz for the phase S. The ansatz (12.35) corresponds to scaling solutions in which the parabolic shape of the density is preserved. The classical radii Ri , where the density (12.35) vanishes, scale in time as 2μ bi (t), (12.37) Ri (t) = Ri bi (t) = mωi2 where Ri are the stationary values of the Thomas–Fermi radii and bi = 1 at equilibrium. By inserting eqns (12.35) and (12.36) into the hydrodynamic equations (12.5) and (12.6), one gets six coupled diﬀerential equations for the time-dependent coeﬃcients bi (t) and αi (t). The parameter n0 (t) is simply determined by the normalization

Large-amplitude oscillations

199

condition obeyed by the density. These equations can be also generalized to include terms xy, yz, and xz in the density (12.35) and in the phase which characterizes the velocity ﬁeld (12.36). This generalization is crucial in the study of rotating condensates. The equation of continuity provides the relationship αi =

b˙ i bi

(12.38)

between the coeﬃcients bi and αi while, using equation (12.6) for the velocity ﬁeld, one ﬁnally ﬁnds the following equation for the scaling parameters bi : ¨bi + ω 2 (t)bi − i

2 ω0i = 0. bi bx by bz

(12.39)

These are three coupled diﬀerential equations which ﬁx the time evolution of the classical radii (12.37) of the order parameter. The second term in (12.39) comes from the conﬁning potential, while the third one originates from the atom–atom interaction. In the small-amplitude limit, eqns (12.39) yields the hydrodynamic frequencies of the normal modes already discussed in Section 12.2. In particular, for axially symmetric traps, expression (12.35) includes the lowest m = 0 and m = 2 modes. When the amplitude of the oscillations grows, there may be a shift of the frequencies as well as a coupling between the diﬀerent modes. An eﬀect which deserves to be mentioned is the large enhancement of nonlinear eﬀects for special values of the asymmetry parameter λ. For certain values of this parameter, it may occur that diﬀerent modes have the same frequency. In the nonlinear regime, one ﬁnds strong mode coupling via harmonic generation when the frequency of a mode becomes equal to one of the second harmonics of other modes. The conditions for this degeneracy can be found numerically by solving eqns (12.39). In the limit of small amplitudes one can also expand the solutions ﬁnding analytical results. In particular, one gets a quadratic shift in the form (Dalfovo et al., 1997b) ω(A) = ω(0)[1 + δ(λ)A2 ],

(12.40)

where A is a parameter related to the amplitude of the oscillation while δ(λ) is an analytic coeﬃcient depending on the anisotropy of the trapping potential and √ on the mode considered. Let us consider, for example, the m = 2 mode where ω(0) = 2ω⊥ . In this mode the radii along x and y oscillate with opposite phase: bx = 1+A cos ωt and by = 1−A cos ωt. The frequency of the collective oscillation is given by eqn (12.40) with δ(λ) =

(16 − 5λ2 ) . 4(16 − 7λ2 )

(12.41)

The divergence at λ = 16/7 is due to the degeneracy between the frequencies of the high-lying m = 0 mode and the second harmonic of the m = 2 mode. In this case, it is diﬃcult to drive the system in a pure mode and, even for relatively small amplitudes, the motion can exhibit a chaotic behaviour. The coeﬃcient δ(λ) can also be calculated for other modes. For √ the low-lying √ √m = 0 mode, for instance, similar divergences are found when λ = ( 125 ± 29)/ 72 (i.e., λ ≈ 0.683 and λ ≈ 1.952).

200

Dynamics of a Trapped Condensate

They occur because the frequency of the high-lying mode becomes equal to the second harmonics of the low-lying mode. Evidence of the mode couplings has been obtained in the experiment of Hechenblaikner et al. (2000).

12.7

Expansion of the condensate

In the previous section we have derived the nonlinear equations (12.39) which provide the time evolution of the radii Ri (t) = Ri (0)bi (t) of the density proﬁles in the Thomas– Fermi approximation. These equations can also be usefully employed to simulate the expansion starting from a gas in equilibrium in the trap, by dropping at a certain time, t = 0, the term ωi2 bi associated with the conﬁning potential. Let us consider the simplest case of an axially symmetric trap and deﬁne b⊥ ≡ bx = by . By introducing the dimensionless time τ = ω⊥ t, with ω⊥ ≡ ωx = ωy , the equation of motion (12.39), after switching oﬀ the trap, takes the form 1 d2 b⊥ = 3 dτ 2 b⊥ bz

(12.42)

d2 λ2 bz = 2 2 , 2 dτ b⊥ bz

(12.43)

and

where λ = ωz /ω⊥ . By solving these equations, one can look, for instance, at the time evolution of the aspect ratio R⊥ /Z = λb⊥ /bz . When τ is large, both b⊥ and bz increase linearly with τ . As a consequence, the parameters α⊥ and αz behave as 1/t and the velocity ﬁeld (12.36) approaches the classical behaviour v = r/t. This result, which also holds beyond the Thomas–Fermi approximation, can be shown by looking at the asymptotic (large t) solution of the equation for the phase (5.15) in the absence of the trapping potential. For large times both the quantum pressure and the interaction term are negligible and the time dependence of the phase is given by S(r) → mr2 /2t. This permits us to write the release energy in the general form m m 2 2 Erel = drv (r, t)n(r, t) drr n(r, t) = . (12.44) 2 2t2 t→∞ t→∞ In Figure 12.6 we show the time evolution of the aspect ratio R⊥ /Z in two cases where accurate experimental data are available. Both traps are cigar-shaped and the number of atoms is large enough to apply the Thomas–Fermi approximation. The agreement between theory (solid lines) and experiments (points) is remarkable. It is worth mentioning that the two equations (12.43) can be solved analytically for λ 1, leading to the useful expressions (Castin and Dum, 1996) b⊥ (τ ) = 1 + τ 2 , (12.45) (12.46) bz (τ ) = 1 + λ2 τ arctan τ − ln 1 + τ 2 . Results (12.45) and (12.46) show explicitly that for elongated condensates the expansion is very diﬀerent in the two directions. While the size of the gas in the direction of

Expansion of the condensate

201

stronger conﬁnement increases fast as a consequence of the repulsive eﬀect associated with the gradient of the density, in the direction of weaker conﬁnement the expansion is slow, being suppressed by the factor λ2 (see eqn (12.46)). This means that even for relatively long times the increase of the size of the condensate in the zth direction remains small. Results (12.45) and (12.46) provide an excellent approximation in many cases of experimental interest and predict the asymptotic result limτ →∞ (R⊥ /Z) = 2/(πλ) for the aspect ratio. In the two conﬁgurations of Figure 12.6, this asymptotic limit is, respectively, 6.5 and 9.7, but is far from being attained in experiments. The above formalism also allows one to calculate the time evolution of the various contributions to the release energy (11.25). In terms of the scaling parameters bi , the release energy takes the form 2μ0 1 b˙ 2i 1 Erel = , (12.47) + N 7 2 i ωi2 bx by bz (a)

(b) 4

Aspect ratio

3

2

1 87Rb

0

0

10

20

Na (MIT)

(Konstanz)

30

40

0 Time [ms]

10

20

30

40

Figure 12.6 Aspect ratio, R⊥ /Z, of an expanding condensate as a function of time. The experimental points in (a) correspond to 87 Rb atoms initially conﬁned in a trap with λ = 0.099 (Ernst et al., 1998). The points in (b) are measurements on sodium atoms, initially in a trap with λ = 0.065 (Stamper-Kurn and Ketterle, 1998). The solid lines are obtained by solving eqns (12.42) and (12.43), which are equivalent to the time-dependent GP equation in the Thomas–Fermi limit. The dashed lines correspond to the λ 1 limit of the same equations, that is to eqns (12.45) and (12.46), and are almost indistinguishable from the solid lines. The dot–dash lines are the predictions for noninteracting atoms.

202

Dynamics of a Trapped Condensate

where the ﬁrst term corresponds to the kinetic energy, while the second one corresponds to the interaction term. The release energy is conserved during the expansion. At t = 0, when bi = 1 and b˙ i = 0, it coincides with the mean-ﬁeld energy. During the expansion the mean-ﬁeld energy is converted into kinetic energy and soon becomes negligible because of the diluteness of the system. The expansion then proceeds at constant speed in each direction. Finally, it is insightful to compare the above results, derived within the framework of hydrodynamic theory, with the predictions of the noninteracting model discussed in Section 10.5. In the ideal gas the asymptotic form of the density proﬁle, after expansion, is entirely ﬁxed by the initial momentum distribution of the gas. The asymptotic anisotropy of the aspect ratio consequently reﬂects the anisotropy (10.43) of the momentum distribution and is given by λ−1/2 . In contrast, in the hydrodynamic approach any information on the initial momentum distribution is lost since this approach neglects the quantum kinetic pressure term. In the hydrodynamic picture the asymptotic behaviour of the density proﬁle reﬂects the anisotropy of the gradient of the pressure term produced by the mean-ﬁeld interaction. The aspect ratio obtained from the dispersion of a free atomic wave packet is represented in Figure 12.6 by the two dot–dash lines. The comparison with experiments shows that the noninteracting model fails to reproduce the experimental data, which are instead well described by the hydrodynamic theory, thereby revealing the crucial role played by the mean-ﬁeld interaction during the expansion.

12.8

Dynamic structure factor

As extensively discussed in Chapter 7, the dynamic structure factor provides an important characterization of the dynamic behaviour of quantum many-body systems. This physical quantity is measurable through inelastic scattering experiments in which the probe particle is weakly coupled to the many-body system so that the scattering may be described within the Born approximation. In Chapter 8 we have already discussed the relevance of neutron scattering experiments in superﬂuid helium. In the case of dilute gases the dynamic structure factor can be measured via inelastic light scattering. The dynamic structure factor provides information on both the spectrum of collective excitations, including the propagation of sound, which can be investigated at low momentum transfer, and the momentum distribution, which instead characterizes the behaviour at high momentum transfer, where the response is dominated by the single-particle motion. Let us recall that the dynamic structure factor is deﬁned by the expression (see eq. (7.31)) S(q, ω) = Q−1 e−βEm | n|δρ†q |m |2 δ(ω − ωmn ), (12.48) mn

where q and ω are the momentum and energy transferred by the probe to the sample and δρq = ρq − ρq eq is the ﬂuctuation of the Fourier component ρq =

N k=1

e−iq·rk

(12.49)

Dynamic structure factor

203

of the density operator. An important quantity, directly related to the dynamic structure factor, is the imaginary part of the response function which, according to the general formalism developed in Chapter 7, can be written as χ (q, ω) = π (S(q, ω) − S(−q, −ω)).

(12.50)

In a trapped gas the quantity χ can be measured using two-photon optical Bragg spectroscopy. The scheme of the experiment is illustrated in Figure 12.7. Two laser beams are impinged upon the condensate. The diﬀerence in the wave vectors of the beams deﬁnes the momentum transfer q, while the frequency diﬀerence deﬁnes the energy transfer ω. Both the values of q and ω can be tuned by changing the angle between the two beams and varying the frequency diﬀerence of the two laser beams. The atoms exposed to these beams can undergo a stimulated light-scattering event by absorbing a photon from one of the beams and emitting into the other. After exposure to these laser beams, the response of the system can by measured by timeof-ﬂight techniques by determining the number of optically excited atoms or the net momentum transfer to the gas. Because atoms can scatter by absorbing a photon from either of the laser beams, the response of the system measures the diﬀerence (12.50) rather than the dynamic structure factor itself. This is an important diﬀerence with respect to other scattering experiments (like neutron scattering from helium) where, by detecting the scattered probe, one measures directly the dynamic structure factor. The dynamic structure factor and the imaginary part of χ have the same behaviour at T = 0, since in this case S(q, ω) is zero for negative ω. However, they diﬀer at ﬁnite k2, ω2

k1, ω1

q

Trapped condensate

Figure 12.7 Schematic representation of a Bragg scattering experiment. Atoms exposed to two detuned laser beams can undergo a stimulated light-scattering event by absorbing a photon with wave vector k1 from one of the beams and emitting a photon with wave vector k2 into the other. The reaction imparts energy ω and momentum q along the axis of the trapped condensate.

204

Dynamics of a Trapped Condensate

temperatures if kB T is higher than the excitation energy ω. The relationship between χ (q, ω) and S(q, ω) is given by χ (q, ω) = π 1 − e−ω/kB T S(q, ω).

(12.51)

Actually the diﬀerence (12.50) signiﬁcantly suppresses the thermal eﬀects exhibited by the dynamic structure factor so that, by measuring χ , one has a useful access to the low-temperature value of S(q, ω) (see Section 7.5). In the following we will address two important questions: i) How are the physical quantities measured in two-photon Bragg scattering experiments related to the imaginary part of the response function and hence to the dynamic structure factor? ii) What are the main features exhibited by the dynamic structure factor of a trapped Bose gas and in particular what is the interplay between the collective and singleparticle phenomena? The ﬁrst question is relevant not only for Bose–Einstein condensed gases, but also for Fermi gases. Let us start our discussion by showing that the eﬀect of two intersecting beams is to create a periodic potential varying in space and time like cos(q·r−ωt). In fact, the electric ﬁeld of the two beams, which separately are supposed to have the same intensity, can be written in the form E(r, t) =

E0 q ω q ω cos K + ·r− Ω+ t + cos K − ·r− Ω− t , 2 2 2 2 2 (12.52)

where Ω ± ω/2 and K ± q/2 are, respectively, the frequency and wave vector of the two lasers. In practice, the frequency diﬀerence ω is always much smaller than Ω, while the diﬀerence q between the two wave vectors can vary between 0 and 2K, depending on the angle between the two beams. Atoms exposed to this intensity modulation experience a potential which can be written in the form (see Section 9.5) 1 U (r, t) = − α (Ω) E 2 (r, t), 2

(12.53)

where α (Ω) is the atomic electric polarizability, which can be safely evaluated at the frequency Ω, neglecting the small detuning ±ω/2. Equation (12.53) is valid for a weak laser ﬁeld, where linear approximation holds, and in the absence of dissipation, so that α (Ω) is real. A simple trigonometric transformation gives E 2 = E02 cos2 (K · r − Ωt) cos2 21 (q · r − ωt) and, since the light frequency Ω is very large with respect to the typical frequencies characterizing the atomic motion in the gas, one can replace cos2 (K · r − Ωt) with its average value 1/2. The potential can ﬁnally be presented in the form U (r, t) = −α (Ω)

E02 cos(q · r − ωt). 4

(12.54)

Dynamic structure factor

205

Notice that, due to the detuning between the two laser beams, the potential felt by the atoms exhibits a time dependence which can induce transitions of energy ω. In practice, in order to obtain a visible eﬀect, one has to work close to the line of the electronic transitions, where the polarizability is large and can be written in the form α (Ω) ∝ 1/(Ω0 − Ω), where Ω0 is the resonance frequency. At the same time the detuning |Ω0 − Ω| should be large compared to the line width, so that α (Ω) is real. By taking the sum over all the atoms we ﬁnally obtain the expression HBragg =

V † −iωt δρq e + δρq eiωt 2

(12.55)

for the Hamiltonian giving the interaction with the laser ﬁeld, where δρq = ρq − ρq is the ﬂuctuation of the density operator (12.49) and V = −αE02 /4 is the strength of the perturbation. This strength can be also written as V = 2ΩR , where ΩR is the so-called two-photon Rabi frequency. Equations (12.53)–(12.55) reveal the ‘classical’ nature of the interaction between atoms and the electromagnetic ﬁeld, which is here treated as a purely classical ﬁeld. This explains why these experiments directly measure the response function rather than the dynamic structure factor. The Bragg pulse starts at some initial time t = 0 and has a ﬁnite duration, as a function of which one can calculate the relevant physical observables. By assuming that the pulse is switched on instantaneously and using the Fourier representation of the step function, the perturbation can be written as i 1 V HBragg = δρ†q dω e−iω t + H.c. (12.56) 2 2π (ω − ω + iη) both for t < 0, where HBragg = 0 (the poles of the integrand lie in the lower part of the complex plane) and t > 0, where (12.56) reduces to (12.55). The energy transfer from the laser beams to the condensate can be easily calculated using the formalism of the linear response function. We can write dE/dt = (1/i)[H, Htot ] = (1/i)[H, HBragg ], where E = H is the expectation value of the Hamiltonian of the system and Htot = H + HBragg . Since the Bragg Hamiltonian depends on the local density, only the kinetic energy term in H contributes to the above commutator which becomes [H, HBragg ] = (V /2)(q · j†q e−iωt − q · jq eiωt ), where jq is the current operator (7.47). Recalling that, as a consequence of the equation of continuity (7.45) one has q · jq = idρq /dt, the energy rate takes the form V dE =− dt 2

d δρq eiωt + c.c. , dt

(12.57)

where the density ﬂuctuation ρq can be calculated by applying linear perturbation theory to the ﬁeld (12.56). By carrying out the integration in the complex plane over the frequencies of the Bragg ﬁeld (12.56), we obtain, for t > 0, the result δρq = −

V −iωt e 2π

dω χ (q, ω )

ei(ω−ω )t − 1 ω − ω

(12.58)

206

Dynamics of a Trapped Condensate

for the density ﬂuctuations induced by the Bragg potential. In deriving (12.58) we have assumed that the ﬂuctuation δρq produced by the e−iω t component of the per turbation (12.56) oscillates like e−iω t and we have neglected the term oscillating like iω t e . The latter term vanishes exactly in a uniform body and is in general exponentially small if the value of q is much larger than the inverse of the size of the system. By eqn (12.58) into eqn (12.57) and making use of the general property inserting dω χ (q, ω ) = 0, one can rewrite the energy rate in the useful form 2 dE = dt π

V 2

2

dω ω χ (q, ω )

sin ((ω − ω )t) , ω − ω

(12.59)

holding for t > 0. Result (12.59) is well suited to exploring the limiting cases of large and small t. In the ﬁrst case (ωt 1) one recovers the golden rule result dE =2 dt

V 2

2

ωχ (q, ω),

(12.60)

where we have used the identity limk→∞ sin(kx)/x = πδ(x). In the opposite limit (t → 0) one instead ﬁnds the result dE = dt

V 2

2

2t π

dω ω χ (q, ω ) =

V 2

2 2t

q2 N, m

(12.61)

where we have used the model-independent f -sum rule (7.48) which, in terms of the imaginary part of the response function, takes the form dωωχ (q, ω) = N q 2 /m. Experimentally, the determination of the energy rate is not always easily accessible. The total momentum transferred by the laser to the condensate is instead easier to detect, by following the motion of the centre of mass of the condensate after the Bragg pulse. At very high momentum transfer both the energy and momentum transfers can be measured by counting the number of atoms scattered by the Bragg pulse carrying energy 2 q 2 /2m and momentum q. The momentum transfer can also be calculated using perturbation theory. However, in this case one cannot ignore the force produced by the harmonic oscillator, which, for large times, aﬀects the amount of momentum accumulated by the condensate. To calculate the momentum rate one starts from N the equation dPz /dt = (1/i)[Pˆz , Htot ], where Pˆz = k=1 pzk and Pz = Pˆz . The commutator equation is easily calculated and one ﬁnds [Pˆz , Htot ] = entering the above 2 † −iωt −imωz k zk + (V /2)q(δρq e − δρq e+iωt ), where the ﬁrst term arises from the oscillator potential, while the second arises from the Bragg perturbation (12.55). By using result (12.58) for the density ﬂuctuation one then derives the following equation for the momentum rate at positive times 2 dPz 2 V sin ((ω − ω )t) 2 = −mωz Z + q dω χ (q, ω ) , (12.62) dt π 2 ω − ω where Z = k zk is the centre-of-mass coordinate. A closed equation for Pz is easily obtained by taking the time derivative of (12.62) and using the exact equation dZ/dt =

Dynamic structure factor

207

Pz /m. Only if the duration of the Bragg pulse is short compared to the oscillator period 2π/ωz will the term proportional to Z in eqn (12.62) be negligible. Furthermore, if the duration of the pulse is at the same time large compared to the inverse of the frequency of the applied ﬁeld, then the equations for the momentum and energy rate become perfectly equivalent and reduce to 1 dPz 1 dE = =2 q dt ω dt

V 2

2

χ (q, ω).

(12.63)

Although restrictive, the conditions ωt 1 and ωz t 1, needed to use the golden rule (12.63) for the momentum rate, can simultaneously be satisﬁed. Even in the phonon regime, where the excitation energy ω should be smaller than the chemical potential μ, the conditions are compatible in large samples where μ ωho (Thomas– Fermi regime). For momenta much larger than the inverse of the healing length (or, equivalently, when ω μ) these conditions can be satisﬁed much more easily. Actually, in this case the energy of the scattered atoms is much larger than the average energy of the atoms in the condensate, so that the rate (12.63) can more easily be measured by just counting the number NBragg of scattered atoms carrying momentum q. In this case one can directly use the equation d 2 NBragg = dt

V 2

2

χ (q, ω)

(12.64)

to extract the response function. It is worth noticing that all the results derived above depend on the combination (12.50) χ (q, ω)) = π(S(q, ω) − S(q, −ω). Since this combination does not depend signiﬁcantly on temperature, provided one is well below Tc , in the following we will restrict our discussion to T = 0. Using procedures similar to the ones described above, the dynamic structure factor of trapped condensates has been measured both in the phonon regime (Stamper-Kurn et al., 1999) and in the so-called large-q impulse regime (Stenger et al., 1999). In the ﬁrst case the experimental value was extracted by analysing the momentum rate, while in the second case it was found by directly measuring the total number of scattered atoms and using relation (12.64). In these experiments the region where the two lasers intersect covers the whole volume of the trapped gas so that the measurements provide information on the global value of the dynamic structure factor. The physical information that one extracts from the dynamic structure factor is very diﬀerent at low and high momentum transfer. Let us start the discussion by recalling that, for large samples and for certain regimes of momentum transfer, one can evaluate the dynamic structure factor of the whole system at zero temperature by employing a local approximation, i.e. by treating the system as if it were locally uniform. By using the Bogoliubov expression S(q, ω) = N

2 q 2 δ (ω − (q)) 2m(q)

(12.65)

208

Dynamics of a Trapped Condensate

for the dynamic structure factor of a uniform interacting gas at T = 0, one can derive a local density approximation (LDA) in the form 2 q 2 SLDA (q, ω) = drn(r) δ (ω − (r, q)), (12.66) 2m(r, q) where n(r) is the ground state density and 2 q 2 2 q 2 + gn(r) (r, q) = 2m 2m

(12.67)

is the Bogoliubov dispersion law calculated at the corresponding density. Equation (12.66) holds at zero temperature and is expected to accurately describe the dynamic structure factor for momenta larger than /R where R is the radius of the condensate, since in this case the eﬀects of discretization in the excitation spectrum can be safely ignored. However, the momentum transfer q should not be too large because the LDA approximation ignores the Doppler eﬀect associated with the spreading of the momentum distribution of the condensate, and this is expected to become the leading eﬀect in the dynamic structure factor at very large q. By inserting the Thomas–Fermi proﬁle (11.7) into eqn (12.66) we obtain the simple analytic formula 15 (ω 2 − ωr2 ) (ω 2 − ωr2 ) SLDA (q, ω) = , (12.68) 1 − 8 ωr μ2 2ωr μ where ωr =

q 2 2m

(12.69)

is the recoil energy and μ is the Thomas–Fermi value (11.8) of the chemical potential. Unlike in the case of a uniform gas the dynamic structure factor is no longer a δ function, its value being diﬀerent from zero in the interval ωr < ω < ωr 1 + 2μ/ωr . The value ω = ωr corresponds to the excitation energy in the region near the border, where the gas is extremely dilute and hence noninteracting. The value ω = ωr 1 + 2μ/ωr is the excitation energy of a Bogoliubov gas evaluated at the central density. Notice that the LDA expression (12.68) for S(q, ω) does not depend on the direction of the vector q, even in the presence of a deformed trap. Starting from eqn (12.68) one can easily calculate the peak energy of the dynamic structure factor. For small q (phonon regime) one ﬁnds the result ωpeak = 2/3cq, where c is the sound velocity of uniform matter calculated at the central density. For large q one instead gets the result 2 ωpeak = ωr + μ, 3

(12.70)

which corresponds to the average of the Bogoilubov energy (12.67) evaluated at large q: (q, r) → 2 q 2 /2m + gn(r). Analogously, one can evaluate the width of the dynamic

Dynamic structure factor

209

structure factor.Using the root mean square deﬁnition Δ = m2 /m0 − (m1 /m0 )2 , with mk = k+1 dωω k S(q, ω) and using expression (12.68) for the dynamic structure factor, one obtains, at large q, the result 8 ΔLDA = μ/, (12.71) 147 which turns out to be independent of q. In Figure 12.8 we show the behaviour of the peak energy, evaluated from eqn (12.68), together with the experimental results of Steinhauer et al. (2002). These measurements provide a nice check of the Bogoliubov dispersion law in a wide range of values of qξ and conﬁrm the validity of the LDA approximation. Actually, when the momentum transfer q becomes large the response of the system is sensitive to the momentum distribution which produces a Doppler broadening, an eﬀect ignored by the LDA expression (12.66). The limit where the response of the system is dominated by the Doppler broadening is called the impulse approximation (IA). In this case the dynamic structure factor takes the form p2 (p + q)2 SIA (q, ω) = dpδ ω − + n(p), (12.72) 2m 2m ˆ † (p)Ψ(p) ˆ where n(p) = Ψ is the momentum distribution of the system. The expression (12.72) for the dynamic structure factor can be also rewritten in the form m SIA (q, ω) = dpx dpy n(px , py , Y ), (12.73) q

ħω/2π [kHz]

18

12 ħ2q 2/2m 6

0

0

1

2

3

qξ

Figure 12.8 Excitation spectrum of a trapped Bose–Einstein condensate of rubidium atoms measured with Bragg scattering (Steinhauer et al., 2002). The solid line is the peak energy calculated in the LDA (see eqn (12.68)). The value μ/2π = 1.9 kHz was used.

210

Dynamics of a Trapped Condensate

where we have assumed that the vector q is oriented along the z axis and Y = (ω − ωr )m/q is the relevant scaling variable of the problem. The integral dpy dpz n(px , py , pz ) is also called the longitudinal momentum distribution. In the IA the peak of S(q, ω) coincides with the recoil energy ωr , while the curve is broadened due to the Doppler eﬀect in the momentum distribution. A useful estimate of the broadening can be obtained using the Thomas–Fermi result (11.18) for the momentum distribution of a Bose–Einstein condensate and carrying out a Gaussian expansion in the dynamic structure factor (12.73) near the peak ωr . The result is (Zambelli et al., 2000)

(ω − ωr )2 , SIA (q, ω) SIA (q, ωr ) exp − 2Δ2IA

(12.74)

where for ΔIA one ﬁnds, after some straightforward algebra, the result ΔIA =

8 q . 3 mRz

(12.75)

Notice that, in contrast to the LDA width (12.71), the width (12.75) increases linearly with the momentum transfer q. Result (12.74) can be used to test the validity of the IA. Figure 12.9 clearly shows that the IA prediction (12.75) is much more adequate than (12.71) for describing the experimental results for the width of the dynamic structure factor at large momentum transfer.

0.09 μ/h = 3.48 kHz

23Na

S(q, ω) × ħω / N

ωr / 2π = 99.65 kHz 0.06

LDA

b = 6.7

0.03 eikonal

IA 0.00 −12

−8

−4

0 4 (ω−ωr)/2π [kHz]

8

12

Figure 12.9 Dynamic structure factor of a trapped condensate at T = 0. The numerical predictions of the eikonal approximation (Zambelli et al., 2000) (solid line), IA (dashed line), and LDA (dotted line) are compared with the experimental data of Stenger et al. (1999). c 2002, American Reprinted with permission from Physical Review Letters, 88, 120407; Physical Society.

Dynamic structure factor

211

The above discussion has shown that there are two important limits where the dynamic structure factor of a trapped Bose gas can be investigated in a simple way. A ﬁrst limit is the local density approximation where the system behaves at each point like a uniform Bogoliubov gas at the corresponding density. This approximation accounts for the mean-ﬁeld eﬀects, which are responsible for the propagation of phonons at small q and for the shift of the peak at high q. Due to the nonuniformity of the medium the dynamic structure factor predicted by the LDA exhibits a width whose value is directly related to the interaction strength and, for large q approaches a constant value, ﬁxed by the chemical potential. A second limit is provided by the impulse approximation, in which the scattering is described in terms of the single-particle motion and of the corresponding Doppler eﬀect associated with the broadening of the momentum distribution. In this approximation the peak energy is given by the recoil energy, while the width of the dynamic structure increases linearly with q. Both the LDA and the IA approximations have been derived in the framework of the Bogoliubov scheme which in principle should describe the correct response for all ranges of momenta. In order to describe the transition between the LDA and IA regimes and to better understand the corresponding conditions of applicability it is useful to evaluate the high-energy solutions by explicitly solving the Bogoliubov equations (12.2) on a more general basis. This can be done in a semi-analytic way by using the formalism of the eikonal expansion. In the following we will only consider the case of large q, where the relevant excitation energies ω are much larger than the chemical potential μ. For smaller values of q (but still large compared to the inverse size of the condensate) the LDA is expected to be the accurate theory. Due to the high value of the energy one can neglect the function v(r) in the ﬁrst equation (12.2) and look for a solution of the form u(r) = exp[ipf · r/]˜ u(r), where pf is the momentum of the excitation carrying energy ωf = p2f /2m and u ˜(r) is a slowly varying function. Retaining only terms with a ﬁrst spatial derivative of u ˜(r) (eikonal approximation), the solution of (12.2) takes the form

z p · r m f exp −i u(r) exp i dz Veﬀ (x, y, z ) , pf 0

(12.76)

where the eﬀective potential Veﬀ (r), calculated in the Thomas Fermi limit, is equal to gn(r) inside and to Vext (r)−μ outside the condensate. At high q the main contribution to the dynamic structure factor (12.48) arises from the excited states with pf ∼ q. This has been taken into account in the eikonal correction u ˜(r) (second factor of eqn (12.76)), where pf was chosen along the z-axis, i.e. the axis ﬁxed by q. Notice that in the eikonal approximation the free-particle solution eipf ·r/ is modiﬁed by the interactions only through a change of the phase. The importance of such a correction in the behaviour of the dynamic structure factor depends on the maximum phase deviation of u(r) from a pure plane wave. The deviation is determined by the so-called Born parameter b=

μ qRz , ωr

(12.77)

212

Dynamics of a Trapped Condensate

where ωr = q 2 /2m and Rz is the Thomas–Fermi radius (11.13) in the direction of the momentum transfer. From the second eqn (12.2) one can obtain the amplitude v, whose inclusion in the equation for u will however result in a higher-order correction. Using result (5.90) for calculating the matrix elements of the density operator, we can now evaluate the dynamic structure factor. If the Born parameter (12.77) is small, the eikonal correction can be neglected and one recovers the IA result (12.72). Conversely, if b is large one ﬁnds a very diﬀerent behaviour. In this case the eikonal phase exhibits large ﬂuctuations which signiﬁcantly change the behaviour of the dynamic structure factor. In the limit b 1 one recovers the LDA result (12.66), in the limit of large q, where (q, r) 2 q 2 /2m + gn(r). Thus the eikonal approach provides the proper description of the dynamic structure factor in all the regimes of momentum transfer ranging from the LDA to the IA, provided ωr μ. It is interesting to notice that the Born parameter (12.77) also ﬁxes the ratio between the widths (12.71) and (12.75) of the dynamic structure factor calculated in the IA and LDA limits, respectively. In fact, one has ΔLDA b , = ΔIA 14

(12.78)

so that the comparison between the two widths provides an equivalent criterion for the applicability of the two opposite approximations. The transition between the LDA and the IA takes place when the ratio (12.78) is close to unity. Using the relation μ = 2 /2mξ 2 , where ξ is the healing length calculated at the centre of the trap, this corresponds to the value q = Rz /14ξ 2 for the momentum transfer. Notice that this value is much larger than /ξ, since in the Thomas–Fermi limit one has Rz ξ. As a consequence, the transition always takes place in the regime of momenta where the Bogoliubov spectrum is dominated by single-particle excitations. Figure 12.9 shows that the eikonal approach provides a rather good prediction and explains the deviation of the observed signal from the LDA as well as from the IA. The width of thedynamic structure factor is in general well reproduced by the quadrature expression Δ2LDA + Δ2IA accounting for both the mean-ﬁeld and Doppler eﬀects. Let us ﬁnally mention that the measurement of the momentum distribution, following the procedures described above, permits us to obtain an important experimental check of the Bogoliubov theory presented in Chapter 4. Let us suppose that at some time we generate in the system a number of Next excitations carrying momentum q. According to eqn (4.43) the momentum distribution of the gas will be modiﬁed by the appearance of the new term ! 2 δn(p) = Next u2q δ(p − q) + vq δ(p + q) . (12.79) Result (12.79) reﬂects the peculiarity of the Bogoliubov transformations (4.23) which predict that, for each elementary excitation carrying momentum q, there are u2 atoms moving with the same momentum q and v 2 atoms moving with opposite momentum −q. This eﬀect is particularly important in the phonon regime, where the amplitudes u and v exhibit the divergent infrared behaviour v 2 → u2 → mc/2q (see eqn (4.28)). According to the theory developed in this section the dynamic structure

Collective versus single-particle excitations

213

factor, measured at high momentum transfer Q (IA regime), will exhibit two new characteristic peaks located at the energies 2 (Q ± q)2 /2m, due to the presence of the terms (12.79) in the momentum distribution (Brunello et al., 2000). By measuring the intensity of these two peaks it is then possible to gain access to the Bogoliubov amplitudes u2 and v 2 . This eﬀect has been investigated experimentally by Vogels et al. (2002).

12.9

Collective versus single-particle excitations

In the previous sections we have discussed the collective excitations of a trapped Bose– Einstein condensate, pointing out the crucial role played by two-body interactions. We may ask whether these collective modes are relevant for the statistical properties of these many-body systems. One knows, for instance, that the thermodynamic behaviour of superﬂuid 4 He is dominated by the thermal excitation of phonons and rotons up to the critical temperature (see Chapter 9). For the trapped gas the situation is very diﬀerent. First, the system is very dilute and one expects the eﬀects of collectivity to be less relevant except at very low temperatures. Second, the harmonic conﬁnement leaves space for excitations of a single-particle nature which are localized near the surface, as we will discuss soon. The simplest way to understand the role of these single-particle excitations is to look at the spectrum obtained by solving numerically the Bogoliubov equation (12.2). In Figure 12.10 we show the eigenstates evaluated for a condensate of 104 atoms of 87 Rb in a spherical trap (Dalfovo et al. 1997a). Each state, having energy ε and angular momentum , is represented by a thick solid bar. For a given angular momentum, the number of radial nodes, i.e., the quantum number nr , increases with energy. By looking at the eigenstates at high energy and multipolarity in the spectrum of the ﬁgure, one notes that the splitting between odd and even states is approximately ωho and the spectrum resembles the one of a three-dimensional harmonic oscillator. Actually, the states with the same value of (2nr + ) would be degenerate in the harmonic oscillator case, while here they have slightly diﬀerent energies, the states with lowest angular momentum being shifted upwards as a result of the mean ﬁeld produced by the condensate in the central region of the trap. The single-particle picture is obtained by neglecting the coupling between the positive (u) and negative (v) frequency components of the order parameter in the Bogoliubov equations (12.2). This corresponds to setting v = 0 in the ﬁrst eqn (12.2), which then reduces to the eigenvalue problem (Hsp − μ)u = ωu, for the single-particle (sp) Hamiltonian Hsp = −

2 2 ∇ + Vext (r) + 2gn0 (r). 2m

(12.80)

In case, the eigenfunctions u(r) satisfy the normalization condition this dr u∗i (r)uj (r) = δij . Once the condensate density n0 and the chemical potential μ are calculated from the stationary GP equation (11.1), the single-particle excitation spectrum of the Hamiltonian (12.80) can be easily calculated. The eigenstates are shown as dashed horizontal

214

Dynamics of a Trapped Condensate 20

Energy [units of ћωho]

15

10 μ

5

N = 10 000 0

0

4

8 12 Angular momentum

16

20

Figure 12.10 Excitation spectrum of 10 000 atoms of 87 Rb in a spherical trap with aho = 0.791 μm. The eigenenergies of the linearized time-dependent GP eqn (12.2) are represented by thick solid bars. Dotted bars correspond to the single-particle spectrum of the Hamiltonian (12.80). The thin horizontal line is the chemical potential μ = 8.41, in units of ωho . From Dalfovo et al. (1997a).

bars in Figure 12.10. One sees that the general structure of the spectrum is very similar to the one obtained with the Bogoliubov equations (12.2), apart from the states with low energy and multipolarity. The lowest levels, with energy well below μ and small angular momentum, are in fact the collective modes discussed in the previous sections. The single-particle spectrum fails to describe these states. It is worth noticing, however, that even below μ there are many states, with relatively high , which are well approximated by the single-particle Hamiltonian (12.80). These excitations are mainly located near the surface of the condensate, where Hsp has a minimum. The existence of such a minimum is evident in the large N limit, where one can use the Thomas–Fermi approximation for the condensate density. In this case, one has Hsp − μ = −

2 2 1 2 ∇ + mωho |r 2 − R2 |, 2m 2

(12.81)

where R is the Thomas–Fermi radius of the condensate and we have taken, for simplicity, a spherical trap. For ﬁnite values of N the minimum of the single-particle potential is rounded (see Figure 12.11). The fact that the Bogoliubov-type spectrum exhibits states of single-particle nature localized near the surface represents an important diﬀerence with respect to the

215

Vsp− μ

Collective versus single-particle excitations

0

0.5

1

1.5

r/R

Figure 12.11 Single-particle potential Vsp − μ = Vext + 2gn0 − μ as a function of the radial coordinate for a typical trapping conﬁguration. The potential exhibits a minimum near the surface (see eqn (12.81)).

uniform Bose gas, where no single-particle states are present at energies lower than the chemical potential. The transition between the collective and single-particle character can be understood in terms of length scales. In fact, an excitation inside the condensate can no longer be phonon-like when its wavelength is of the order of, or shorter than, the healing length. This happens for states with a large number of radial nodes and energy larger than μ. Conversely, for states localized mainly at the surface, the appropriate length scale is the surface thickness d (see eqn (11.29)). In this case, excitations cannot be collective if their wavelength is smaller than d. This happens when their angular momentum is larger than ∼ R/d ∼ N 4/15 . This critical value of corresponds to an energy of the order of μ(aho /R)4/3 , so that the transition from the collective to the single-particle behaviour occurs at energies smaller than μ in states with high multipolarity. These states can be viewed as atoms rotating in the outer part of the condensate. In order to discuss the relevance of single-particle excitations in the statistical behaviour of these trapped Bose gases it is useful to evaluate the density of elementary excitations. For a ﬁnite system one can easily count the number of available states, with energy ε and angular momentum , each one multiplied by its degeneracy (2 + 1), up to a given energy ε: N (ε) = (2 + 1) . (12.82) ε Tc ), interaction eﬀects are less important because the system is very dilute. In this case one can estimate the interaction energy

Role of interactions, scaling, and thermodynamic limit

219

2 1/2 using the expression Eint /N gN/RT3 , where RT = (2kB T /mωho ) is the classical radius of the thermal cloud. For temperatures of the order of Tc one ﬁnds

a Eint ∼ N 1/6 ∼ η 5/2 . N kB Tc0 aho

(13.4)

This ratio depends on a higher power of η as compared to the analogous ratio (13.2) involving the interaction energy at zero temperature. As a consequence interaction eﬀects, as expected, are much smaller above Tc . The above discussion emphasizes the importance of the dimensionless parameter (13.2), which can be used to discuss the eﬀects of interactions on the thermodynamic behaviour of the system at both low and high temperatures. Actually, in the thermodynamic limit the system exhibits a scaling behaviour on this parameter. The thermodynamic limit for the noninteracting gas conﬁned in a harmonic trap has already been discussed, in Section 10.4. This limit is reached by letting the total number of particles N increase to inﬁnity and the oscillator frequency ωho decrease to zero, with the product ωho N 1/3 kept ﬁxed, where ωho is the geometrical average of the three frequencies. This procedure provides a natural extension of the usual thermodynamic limit holding in uniform systems in which one takes N → ∞, V → ∞, and keeps the density n = N/V ﬁxed. In harmonic traps the quantity ωho N 1/3 represents, together with T , the relevant thermodynamic parameter of the system and replaces the role played by the density in uniform systems. In particular, it ﬁxes the value of the critical temperature (13.1). In the thermodynamic limit all the thermodynamic properties of the noninteracting model can be expressed in terms of the critical temperature Tc0 and the reduced temperature t = T /Tc0 . Of course, dimensionless quantities, like the condensate fraction or the entropy per particle, will depend only on the reduced temperature t. The thermodynamic limit discussed above also holds in the presence of repulsive interactions. In fact, the parameter η deﬁned by eqn (13.2) can be conveniently rewritten in the form 1/5 kB Tc0 η = 1.59 , (13.5) 2 /ma2 which shows that, for a given choice of a, its value is determined by the transition temperature Tc0 and is consequently well deﬁned in the thermodynamic limit. In the same limit the dimensionless Thomas–Fermi parameter N a/aho , which characterizes the eﬀects of two-body interactions in the Gross-Pitaevskii equation for the ground state, behaves like N a/aho ∼ N 5/6 η 5/2 , becoming increasingly large as N → ∞. This means that in the thermodynamic limit the Thomas–Fermi parameter drops out of the problem and all the relevant quantities will depend on Tc0 , t, and η. For example, the chemical potential can be written in the form μ = kB Tc0 f (t, η),

(13.6)

where f is a dimensionless function depending on the reduced temperature t = T /Tc0 and on the scaling parameter η. Similar arguments apply to the other thermodynamic

220

Thermodynamics of a Trapped Bose Gas

functions. A peculiar consequence of interactions is that, in contrast to the ideal gas, where the ratio R0 /RT between the condensate and the thermal radii behaves like (kB T /ωho )1/2 (see eqn (10.28)) and hence tends to zero in the thermodynamic limit, the same ratio now approaches a ﬁnite value. In fact the radius of the condensate 2 and hence one has R /R ∼ scales like R0 ∼ μ/mωho tf (t, η). 0 T An important question is to understand whether, in the available experimental conditions in which N ranges between 104 and 107 , the thermodynamic limit is reached in practice or whether ﬁnite-size eﬀects are still signiﬁcant. Numerical investigations indicate that the scaling limit is already reached with good accuracy for N ∼ 104 −105 . For this reason, in the following we will discuss the behaviour of interacting Bose gases conﬁned in harmonic traps, calculating directly the various physical quantities in the thermodynamic limit.

13.2

The Hartree–Fock approximation

In Section 12.9 we have shown that at zero temperature the excitation spectrum of a trapped condensate is well described by the single-particle Hamiltonian (12.80), apart from eﬀects of collectivity which are important only at very low energies. The form of this Hamiltonian is ﬁxed by the density proﬁle of the condensate which generates a repulsive potential. At ﬁnite temperatures one expects some signiﬁcant changes. First, the condensate density is modiﬁed due to thermal depletion. Second, interaction eﬀects involving the thermal component should be taken into account. The simplest theory which accounts in a self-consistent way for the above eﬀects is the Hartree-Fock (HF) approximation (Goldman et al., 1981; Huse and Siggia, 1982). A natural way to derive the corresponding equations is to start from the many-body Hamiltonian (5.83) 2 2 ˆ = drΨ ˆ † − ∇ + Vext Ψ ˆ †Ψ ˆ + g drΨ ˆ †Ψ ˆ Ψ, ˆ H (13.7) 2m 2 and to write the ﬁeld operator in the form ˆ ϕi (r)ˆ ai , Ψ(r) =

(13.8)

i

ˆ† and a ˆ are where ϕi (r) are single-particle wave functions normalized to unity, and a the usual single-particle creation and annihilation operators. The HF approximation consists of assuming that, at equilibrium, the system can be described as a gas of statistically independent single-particle excitations with average occupation number ni = ˆ a†i a ˆi .

(13.9)

Consistent with the notation used in the previous chapters, the occupation number of the i = 0 state (condensate) will be indicated with N0 ≡ ni=0 . The rule for calculating the energy E = H in the HF approximation is simple. One retains only the terms containing an even number of particle operators and then sets ˆ a†i a ˆk = ni δik

(13.10)

The Hartree–Fock approximation

221

and ˆ†j a ˆk a ˆl = ni nj (δik δjl + δil δjk ) ˆ a†i a

(13.11)

ˆ†i a ˆi a ˆi = ni (ni − 1). Terms like ˆ a†i a ˆ†i or for i = j. When i = j one has to use ˆ a†i a ˆ ai a ˆi , which play a crucial role in the derivation of the Bogoliubov equations, vanish in the HF approximation. It is now easy to calculate the various terms of the energy. By separating the condensate (i = 0) from the excitation states (i = 0) one obtains the result ⎡ 2 2 E = dr ⎣ N0 |∇ϕ0 |2 + ni |∇ϕi |2 + Vext (r) (n0 (r) + nT (r)) (13.12) 2m 2m i=0

+

g n0 (r)2 + 2gn0 (r)nT (r) + gnT (r)2 , 2

(13.13)

where n0 (r) = N0 |ϕ0 (r)|2 = |Ψ0 (r)|2 is the condensate density ﬁxed by the order parameter Ψ0 = nT (r) = ni |ϕi (r)|2

(13.14) √ N0 ϕ0 , while (13.15)

i=0

is the thermal density. Actually, in the calculation of the interaction energy of the condensate (term in n20 (r)) we have assumed N0 1, while in the calculation of the interaction term with i, j = 0 we have also used eqn (13.11) when i = j. These approximations introduce small corrections of order 1/N . Equation (13.13) shows that the expectation value of the interaction term is not simply given by (g/2) n2 dr, as happens at T = 0. This is the consequence of exchange eﬀects, which aﬀect the thermal contribution to the energy and the two-body correlation function (see also Section 3.3). In particular, above Tc the energy is given by g n2 dr. The average occupation numbers ni , as well as the single-particle wave functions ϕi , are determined by minimizing the grand canonical potential E − T S − μN , where N = i ni and, consistently with the assumption of statistical independence of the single-particle excitations, the entropy is calculated using the ideal Bose gas formula S = kB [(1 + ni ) ln(1 + ni ) − ni ln ni ]. (13.16) i

Equivalently, one can minimize the energy at constant entropy and N . Since S depends only on the occupation numbers ni , the single-particle wave functions ϕi are simply obtained by minimizing the energy (13.13) with the proper normalization constraint dr|ϕi |2 = 1 for each value of i. This yields the Schr¨odinger-like equations δE = ni i ϕi , δϕ∗i

(13.17)

222

Thermodynamics of a Trapped Bose Gas

where i physically represents the energy of the ith single-particle level. Equation (13.17) also applies to the i = 0 state for which ni=0 = N0 . Within the same Hartree-Fock scheme the important identity i =

δE δni

(13.18)

holds. With the help of the above equations it is now immediate to carry out the variation δ(E − T S − μN )/δni = 0, which yields the standard result ni =

1 exp β(i − μ) − 1

(13.19)

of Bose–Einstein statistics. The mechanism of Bose–Einstein condensation now proceeds according to the general rules of the independent-particle model. BEC starts when the chemical potential approaches the energy 0 of the lowest single-particle energy. In this case the Schr¨ odinger equations (13.17) takes the form (Goldman et al., 1981; Huse and Siggia, 1982) 2 2 ∇ − + Vext (r) + g[n0 (r) + 2nT (r)] Ψ0 = μΨ0 (13.20) 2m for the condensate wave function Ψ0 , and 2 2 ∇ − + Vext (r) + 2gn(r) ϕi (r) = i ϕi (r) 2m

(13.21)

for the excited single-particle states. Equations (13.19)–(13.21), together with the normalization constraint N = drn(r) = dr (n0 (r) + nT (r)), (13.22) provide the complete (Hartree-Fock) set of equations, which should be solved in a self-consistent way. Some important remarks are in order here: (i) The equation for the order parameter approaches, at T = 0, the stationary GP eqn (11.1), which can consequently be regarded as a Hartree-Fock equation for the ground state. At ﬁnite temperatures, eqn (13.20) includes the interaction with the thermal component. Notice that the combination which characterizes the interaction term in this equation is given by n0 + 2nT . As already pointed out, the factor 2 arises from the exchange term in the calculation of H. (ii) The equation for the single-particle excitations generalizes the T = 0 result (12.80), where the condensate density is now replaced by the total density. In a uniform system (Vext = 0) eqn (13.20) provides the simple result μ = g(n0 + 2nT )

(13.23)

Shift of the critical temperature

223

Chemical potential μ/kBTc

0.6

0.3 Hartree–Fock 0 Ideal –0.3 Bose, gn/kBTc = 0.3 –0.6

0

0.5

1 Temperature T/Tc

1.5

2

Figure 13.1 Chemical potential of a uniform Bose gas as a function of T , calculated from the Hartee–Fock prediction (eqn (13.23)) with gn/kB Tc = 0.3. The ideal gas prediction is also shown. From Papoular et al. (2012).

for the chemical potential below Tc . Above TC eqn (13.20) is not relevant and eqn (13.21) provides the result μ = μIBG + 2gn,

(13.24)

where μIBG is the ideal Bose gas value of the chemical potential. The temperature dependence of the chemical potential, for a ﬁxed value of the density, is shown in Figure 13.1 and exhibits a nonmonotonic behaviour, responsible for a peculiar thermomechanical eﬀect (Papoular et al., 2012). In particular, the chemical potential increases by a of factor 2 when the temperature goes from T = 0 to T = Tc0 . We have already pointed out that in a trapped gas the condensate and the thermal densities have very diﬀerent shapes. As a consequence, the thermodynamic behaviour of such systems can exhibit rather diﬀerent features with respect to the uniform gas. Finally, let us remark that the solutions of the Hartree-Fock eqns (13.20) and (13.21) are not orthogonal since the interaction terms in the corresponding effective Hamiltonians are diﬀerent. This diﬃculty can be solved by explicitly imposing the orthogonality condition on the wave functions φi in the variational derivation. This introduces additional nonlocal terms which modify the eﬀective Hamiltonian of the Hartree-Fock equations (Huse and Siggia, 1982). The resulting corrections affect only a limited number of states and can be neglected in the calculation of the thermodynamic properties of the system.

13.3

Shift of the critical temperature

As anticipated in the previous section, at the onset of BEC the system is very dilute and one does not expect large corrections to the critical temperature due to

224

Thermodynamics of a Trapped Bose Gas

two-body interactions. Nevertheless, the role of interactions on the critical phenomena is an important question from a conceptual viewpoint. It is interesting to understand, in particular, the diﬀerences between the behaviour of uniform and nonuniform Bose gases. In the noninteracting model the system can be cooled, remaining in the normal phase, down to the temperature Tc0 , which satisﬁes the condition n(0)λ3Tc = ζ(3/2) 2.61. Here λT = [2π2 /(mkB T )]1/2 is the thermal wavelength and n(0) is the density at the centre of the trap, which, at the critical temperature, can be evaluated by setting T = Tc0 in eqn (10.27). The presence of repulsive interactions has the eﬀect of expanding the atomic cloud, with a consequent decrease of density. Lowering the peak density then has the eﬀect of lowering the critical temperature. This eﬀect is absent in the case of a uniform gas where the density is kept ﬁxed. The shift in the critical temperature in a trapped gas can easily be estimated by treating the interaction in the mean-ﬁeld approximation. The simplest scheme is the Hartree-Fock theory developed in the previous section. In this theory the motion of thermal atoms is described by the single-particle Hamiltonian (see eqn (13.21)) Hsp = −

2 ∇2 + Vef f (r), 2m

(13.25)

where Vef f = Vext + 2gn(r)

(13.26)

plays the role of an eﬀective potential. If kT ωho one can use the semiclassical expression np (r) =

exp[(p2 /2m

1 + Vef f (r) − μ)/kB T ] − 1

(13.27)

for the particle distribution function of the thermal component, which generalizes the free-particle result (10.26). Integration in momentum space yields the expression 1 nT (r) = 3 g3/2 e−(Veff (r)−μ)/kB T (13.28) λT for the thermal density. Bose–Einstein condensation starts at the temperature for which the normalization condition N = dr nT (r, Tc , μc ) (13.29) can be satisﬁed, with the value of the chemical potential μc corresponding to the lowest eigenvalue of the Hamiltonian (13.25). For large systems the leading contribution arises from interaction eﬀects and can easily be obtained by neglecting the kinetic energy in eqn (13.25). This yields μc = 2gn(0).

(13.30)

Shift of the critical temperature

225

Furthermore, if one works to the lowest order in g (dilute gas approximation), one can calculate the central density n(0) using the noninteracting model. Equation (13.30) clearly ignores ﬁnite-size eﬀects originating from the kinetic energy. By expanding the right-hand side of (13.29) around μc = 0 and Tc = Tc0 , one obtains the following result for the shift δTc = Tc − Tc0 of the critical temperature (Giorgini, Pitaevskii, and Stringari, 1996): δTc a 1/6 = −1.32 N = −0.43η 5/2 , Tc0 aho

(13.31)

where, in the second equality, we have introduced the scaling parameter (13.2). To lowest order in the coupling constant, the shift of Tc is hence negative (we assume a > 0) and linear in the scattering length. The relative shift (13.31) can also be written in the form δTc /Tc0 = −3.43a/λ0 , where λ0 = 2.6aho is the thermal wavelength calculated at the critical temperature (13.1). It has been measured with good accuracy in harmonically trapped Bose gases by Gerbier et al. (2004) and, more recently, by Smith et al. (2011), conﬁrming the mean-ﬁeld prediction (13.31) for small values of the ratio a/aho (see Figure 13.2).

0

∆Tc/Tc0 (%)

–2

–4

–6 Mean-field prediction –8 0.00

0.01

0.02

0.03

0.04

a/ λ0

Figure 13.2 Interaction shift of the critical temperature. Data points were taken with N ≈ 2 × 105 (circles), 4 × 105 (squares), and 8 × 105 (triangles) atoms. The dashed line is the mean-ﬁeld result ΔTc /Tc0 = −3.426 a/λ0 . The solid line shows a second-order polynomial ﬁt to the data. Vertical error bars show standard statistical errors. Horizontal error bars reﬂect the 0.1 G uncertainty in the position of the Feshbach resonance. From Smith et al. (2011). c 2011, American Reprinted with permission from Physical Review Letters, 106, 250403; Physical Society.

226

13.4

Thermodynamics of a Trapped Bose Gas

Critical region near Tc

In the mean-ﬁeld approach discussed in the previous section, the relation between Tc and the critical density in the centre of the trap remains the same as for the noninteracting model. In fact, according to eqns (13.28) and (13.30), one has μc = Vef f (0) and eqn (13.28) yields the relationship n(0)λ3Tc = 2.61. It is interesting to look for eﬀects which violate this relation. These can be either ﬁnite-size or manybody eﬀects beyond-mean-ﬁeld theory. In general, one expects that the deviations from mean-ﬁeld theory will be important near the transition point, in the so-called ‘critical region’. The eﬀects of many-body correlations near Tc have been the object of systematic theoretical work in the uniform gas in recent years, using a variety of approaches based on Path Integral Monte Carlo simulations, renormalization group theory, etc. A ﬁrst important question is to understand whether the leading correction to Tc is linear in the scattering length a. We present here a brief discussion based on general considerations. First of all, one should notice that in the mean-ﬁeld approximation the distribution function (13.27) of a uniform gas is simply obtained from the one of the ideal gas by substituting the chemical potential μ with the renormalized expression μ ˜ = μ− 2gn. The onset of BEC in the mean-ﬁeld picture then corresponds to the condition μ ˜ = 0. However, the mean-ﬁeld approach is not applicable for small μ ˜ because of the occurrence of critical ﬂuctuations. By using perturbation theory one can calculate the ﬁrst corrections to thermodynamics due to these ﬂuctuations. It occurs that these corrections are small if the Ginzburg-like condition 2 m3 g 2 kB Tc0 |˜ μ| 6

(13.32)

is satisﬁed (see, for example, Landau and Lifshitz, 1980, §146). Here kB Tc0 = 3.312 n2/3 /m is the critical temperature (3.28) of the ideal uniform gas (not to be confused with the critical temperature in the trap). If the condition (13.32) is not satisﬁed, many-body eﬀects become important. They change, in particular, the behaviour of the momentum distribution in the region of small momenta where 2 p2 /2m ≤ m3 g 2 kB Tc0 /6 , corresponding to

p ≤ pc ≡

gm2 kB Tc0 . 3

(13.33)

The same argument also suggests that the critical value μ˜c is of the order of 2 m3 g 2 Tc0 /6 . Using the above considerations one can estimate the many-body correction to the critical temperature in a uniform gas. If one works at ﬁxed density, the critical temperature Tc = Tc0 + δTc can be calculated by imposing the condition n (˜ μc , Tc ) = n0 0, Tc0 = Tc − δTc , where n and n0 are ﬁxed by the equation of

Critical region near Tc

227

state in the interacting and ideal gas, respectively. By expanding n0 (0, Tc − δTc ) ≈ n0 (0, Tc ) − 32 nδTc /Tc , one obtains the equation 3 δTc n = 2 Tc0

n0p − np

dp (2π)

3,

(13.34)

where we have expressed the densities n (˜ μc , Tc ) and n0 (0, Tc ) as integrals of the corresponding momentum distributions np and n0p , and we have set n0 ∼ n in the left-hand side. The order of magnitude of the right-hand side of this equation can be estimated by noticing that the crucial contribution to the integral arises from the small values p ∼ pc . For larger momenta the eﬀects of the interaction can be neglected. When p ∼ pc , both np and n0p are of the order of kB Tc m/p2c , but there is no exact cancellation between the two terms. By multiplying this quantity by dp ∼ p3c one ﬁnally ﬁnds that the relative shift of the critical temperature follows the law (Baym et al., 1999) δTc kB Tc0 mpc ∼ ∼ an1/3 . 0 Tc n3

(13.35)

The fact that the shift of Tc in the uniform gas is predicted to be linear in the scattering length is not at all a trivial result and diﬀerent predictions have been formulated in the past for such an eﬀect (for a review discussion see Baym et al., 2000, 2001 and Arnold and Moore, 2001). Also, the mean-ﬁeld shift (13.31) of Tc in the presence of a harmonic trap is linear in a. However, the physical origin of the eﬀect is completely diﬀerent in the two cases. The above arguments do not provide an analytic way to estimate the value of the coeﬃcient of an1/3 , and even the sign cannot be predicted with simple arguments. The coeﬃcient was estimated by Baym et al. (1999) using diagrammatic techniques. A safer quantitative estimate is provided by Monte Carlo simulations, which give the result (Kashurnikov et al., 2001; Arnold and Moore, 2001) δTc = 1.3an1/3 . Tc0

(13.36)

Result (13.36) applies to a uniform gas, but cannot be used in the presence of harmonic trapping. Actually, it is possible to show that in this case the inclusion of many-body eﬀects results in higher-order corrections in the coupling constant. This can be understood by noticing that the region aﬀected by the critical behaviour discussed above is restricted to a small volume near the centre of the trap. Furthermore, in the presence of trapping it is possible to show that the many-body correction to Tc is no longer linear, but behaves like a2 log a (Arnold and Tom´ a˘sik, 2001). In conclusion, the leading correction to the critical temperature in the presence of harmonic trapping is dominated by the mean-ﬁeld eﬀect (13.31), while the inclusion of critical ﬂuctuations provides only higher-order corrections.

228

13.5

Thermodynamics of a Trapped Bose Gas

Below Tc

Below the critical temperature Tc , Bose–Einstein condensation results in a sharp enhancement of the density in the central region of the trap. This makes interaction eﬀects much more important than for temperatures above Tc , as discussed in Section 13.1. We start our discussion by considering the perturbative scheme developed in Section 13.2, based on Hartree-Fock theory. As a consequence of the harmonic trapping the thermal density nT is much smaller than the condensate density n0 , even if the fraction of atoms in the thermal cloud is comparable to N0 , and can consequently be neglected in eqn (13.20) (this is a major diﬀerence with respect to the uniform gas). As a result, as long as N0 (T )a/aho 1 the Thomas–Fermi approximation (11.7) also provides a good description for the condensate density at ﬁnite temperatures. Equation (11.8) then permits us to estimate the temperature dependence of the chemical potential, whose value is ﬁxed by the number of atoms in the condensate. One ﬁnds 2/5 N0 μ(N0 , T ) μ(N, T = 0) = ηkB Tc0 (1 − t3 )2/5 , (13.37) N where we have used deﬁnition (13.2) for η and the noninteracting prediction N0 = N (1−t3 ) for the number of atoms in the condensate. The inclusion of corrections to this law would yield higher-order eﬀects. Equation (13.37) provides a useful estimate of μ, which is expected to be accurate in the range μ < T < Tc0 . For smaller temperatures, eqn (13.37) misses the thermal contributions arising from collective excitations. These eﬀects give rise, however, to very small corrections and will be ignored in the present discussion. Above Tc interactions provide corrections of order η 5/2 to the ideal Bose gas prediction for the chemical potential and can also be ignored in ﬁrst approximation. In Figure 13.3 we show the prediction for the temperature dependence of the chemical potential evaluated using the self-consistent Popov (1965) approximation (see, for example, Griﬃn, 1996), which provides very similar results to Hartree-Fock theory in the region of temperatures μ < kB T < Tc . It is worth noticing the diﬀerent behaviour exhibited by the chemical potential with respect to the uniform gas (see Figure 13.1) and in particular the absence of the nonmonotonic dependence. Let us now discuss in more detail the behaviour of the condensed and thermal components of the gas. At high temperatures the thermal part can be treated as a gas of free particles governed by the eﬀective mean-ﬁeld potential Vef f (r) of eqn (13.26). The form of this potential can be further simpliﬁed by ignoring the contribution to the density n(r) due to the dilute thermal component and by evaluating the condensate density in the Thomas–Fermi approximation. This yields the simple result Vef f (r) − μ = |Vext (r) − μ|,

(13.38)

which shows that the eﬀective potential coincides with the trapping potential Vext outside the condensate, where n ∼ 0, while it is drastically changed inside where it becomes repulsive (see also Figure 12.11). In practice, most of thermal atoms occupy regions of space lying outside the condensate, where Vext > μ and Vef f = Vext . However, this does not mean that interaction eﬀects are negligible. In fact, the chemical

Below Tc

229

μ/k BT 0c

0.5

0

−0.5

−1

0

0.4

0.8

1.2

T /T 0c

Figure 13.3 Chemical potential of a harmonically trapped Bose gas as a function of T /T0c in the thermodynamic limit (see text). The dotted line refers to the noninteracting case (η = 0), while the solid and dashed lines refer to η = 0.4 and 0.6, respectively.

potential (13.37) is quite diﬀerent from the noninteracting value and the contribution of thermal atoms to the thermodynamic averages is consequently very diﬀerent. Using the semiclassical result (13.27) one can easily evaluate the number of atoms out of the condensate: 1 drdp NT = . (13.39) (2π)3 exp[(p2 /2m + Vef f (r) − μ)/kB T ] − 1 Explicit integration of (13.39), using the Thomas–Fermi approximation (13.38) for the eﬀective mean-ﬁeld potential, leads to the result N0 ζ(2) 2 = 1 − t3 − ηt (1 − t3 )2/5 , N ζ(3)

(13.40)

which is valid to the lowest order in the interaction parameter η. Equation (13.40) shows that the eﬀects of the interaction on the condensate fraction depend linearly on η and are consequently expected to be much larger than the ones exhibited by the shift of the critical temperature (13.31), which behave like η 5/2 . For example, taking η = 0.4 and t = 0.6 one ﬁnds that interactions reduce the value of N0 by 20% as compared to the prediction of the noninteracting model. The quenching of the condensate fraction due to the interactions is a peculiar feature of trapped Bose gases and takes place because the thermal component of the gas is, in large part, spatially separated from the condensate. In a uniform system one observes an opposite eﬀect. In fact, in this case, the condensate and the thermal components completely overlap and the eﬀective potential is enhanced due to the interaction term 2gn in the eﬀective interaction. This eﬀect is only partially compensated for by the presence of

230

Thermodynamics of a Trapped Bose Gas

the chemical potential and the ﬁnal result is a suppression of the thermal component with consequent increase of the condensate fraction with respect to the ideal case. Result (13.40) can also be written in the useful form ζ(2) μ(N0 , T ) NT , =1+ Nc ζ(3) kB T

(13.41)

where Nc = N t3 = ζ(3)(kB T /ωho )3 is ideal gas model prediction for the number of thermal atoms for T ≤ Tc (see equations (10.10) and (10.11)). Equation (13.41) is particularly useful in discussing the violation of saturation caused by interactions. Without interactions (η = 0) the number NT of thermal atoms, below Tc depends uniquely on the temperature, and if one adds more particles at ﬁxed T they will all be Bose–Einstein condensed. In the presence of interactions part of the added particles will instead become thermal, thereby violating the saturation property predicted by the ideal gas. The eﬀect has been experimentally investigated by Tammuz et al. (2011) and the experimental results are reported in Figure 13.4, together with the prediction of eqn (13.41). It is worth pointing out that the violation of saturation due to interactions is particularly important in harmonically trapped Bose gases where interaction eﬀects, at ﬁnite temperatures, scale like η and hence like a2/5 . In uniform matter the eﬀects are expected to scale linearly with a and are hence much smaller. Schmidutz et al. (2014)

300

Saturated gas

200

BE C

N', N0 (thousands)

Nc

100

0

0

100

200

300

400

N (thousands)

Figure 13.4 Lack of saturation of a quantum degenerate atomic Bose gas. N ≡ NT (upper points) and N0 (lower points) versus the total atom number N at a temperature T = 177 nK and a scattering length a = 135 a0 . The corresponding theoretical predictions, based on eqn (13.41), are also shown (solid lines). The critical point N = Nc is marked by a vertical dotted line. From Tammuz et al. (2011). Reprinted with permission from Physical Review c 2011, American Physical Society. Letters, 106, 230401;

Below Tc

231

have shown actually experimentally with excellent accuracy that the weakly interacting uniform Bose gas exhibits saturation. In a similar way one can calculate the energy of the system as well as all the other thermodynamic quantities. The main eﬀects of temperature and interactions are twofold. On one hand, the number of atoms in the condensate is reduced at ﬁnite temperatures and the density in the central region of the trap decreases. As a consequence the atom cloud becomes larger but more dilute and the interaction energy is reduced as compared to the zero-temperature case. On the other hand, the particles out of the condensate are distributed with a modiﬁed Bose factor as in (13.39). By explicitly calculating the two contributions, one ﬁnds that the total energy of the system exhibits the following temperature dependence: E 3ζ(4) 4 1 t + η(1 − t3 )2/5 (5 + 16t3 ). = N kB Tc0 ζ(3) 7

(13.42)

Notice that the contribution of the interaction, which is again linear in η, can be obtained more directly starting from result (13.37) for the chemical potential by integrating the thermodynamic equation ∂μ ∂E =μ−T , ∂N ∂T

(13.43)

which follows from the relationship ∂S/∂N = −∂μ/∂T . Analogously to eqns (13.37) and (13.40), expression (13.42) is valid in the temperature regime μ < T < Tc and to lowest order in the parameter η. Another useful quantity is the release energy, which corresponds to the energy of the system after switching oﬀ the trap. Using the same approximations discussed above, one ﬁnds the result Erel 17 3 E − Eho 3ζ(4) 4 1 3 2/5 t η(1 − t t 2 + . ≡ = + ) N kB Tc0 N kB Tc0 2ζ(3) 7 2

(13.44)

The release energy can be extracted from time-of-ﬂight measurements and, consequently, the comparison with theory permits us to check experimentally the eﬀects of two-body interactions at ﬁnite temperatures (see Figure 13.5). The mean-ﬁeld approach can also be used to calculate the density proﬁle of the trapped gas at ﬁnite temperatures. A typical prediction is shown in Figure 13.6, in fair agreement with experiments. Expansions similar to the ones discussed in this section can also be carried out in the opposite limit of low temperatures t < η, which is the analogue of the phonon regime of uniform superﬂuids. Though this regime is not easy to study experimentally, its theoretical investigation is rather interesting. The lowtemperature properties of trapped Bose gases are in fact strongly inﬂuenced by the thermal excitation of the single-particle states localized near the surface of the condensate (Giorgini et al., 1997a).

232

Thermodynamics of a Trapped Bose Gas

Release energy

2

1

0

0

0.4

0.8

1.2

T /Tc0

Figure 13.5 Release energy as a function of T /T0c in the thermodynamic limit. The curves refer to the same values of η as in Figure 13.3. Solid circles are the experimental data of Ensher et al. (1996). Reprinted with permission from Physical Review Letters, 77, 4984; c 1996, American Physical Society.

Column density [103 μm−2]

5 4 3 2 1 0

−400

−200

0

z [μm]

200

400

Figure 13.6 Axial proﬁles of a cloud of sodium atoms at two diﬀerent temperatures. The experimental data (solid line) are from Stamper-Kurn and Ketterle (1998) for the temperature T = 0.7 μK. The theoretical curve (dotted line) was obtained by solving the Popov equations (see text) using N and T as ﬁtting parameters: T = 0.8 μK and N = 1.4 × 107 . From Dalfovo et al. (1999).

Equation of state and density proﬁles

233

At ﬁnite temperatures one can derive exact results for the thermodynamic behaviour through quantum Monte Carlo calculations for a Bose gas of hard spheres. First calculations in this direction were carried out by Krauth (1996). The results of the quantum simulation, concerning the temperature dependence of the condensate fraction and the density proﬁles, turn out to be in close agreement with the predictions of the mean-ﬁeld approach.

13.6

Equation of state and density proﬁles

In the previous sections we have discussed the thermodynamic behaviour of an interacting Bose gas in the presence of an external trapping potential. We have presented the predictions of the mean-ﬁeld approach concerning the density proﬁle as well as the eﬀect of the interactions on the value of the critical temperature. The thermodynamic behaviour of the trapped gas can also be investigated by employing an alternative approach, based on the knowledge of the equation of state of uniform matter and on the use of the so-called local density approximation (LDA). For large systems one in fact expects that, locally, the system can be treated as a piece of uniform matter and that its chemical potential μ0 can consequently be written as the sum of the value μ[n(r, T )] of the chemical potential, evaluated in uniform matter at the local value of the density, and of the external potential Vext : μ0 = μ(n, T ) + Vext (r).

(13.45)

Equation (13.45) then provides an implicit equation for the density proﬁle n(r, T ) of the trapped gas at a given temperature T . The value μ0 is ﬁxed by the normalization condition N = n[μ0 − Vext (r), T ]dr, (13.46) which permits us to determine the thermodynamics of the trapped gas in terms of the thermodynamic behaviour of the uniform system (Damle et al., 1996). The LDA result (13.45) can also be derived starting from the variational procedure

δ

dr {[n(r)] − T s(r) + Vext (r)n(r) − μ0 n(r)} = 0,

(13.47)

applied to the grand canonical potential calculated in the local density approximation, where [n(r, T )] and s[n(r, T )] are the energy and entropy densities, respectively, and we have used the thermodynamic relation μ(n) = (∂ ((n) − T s(n)) /∂n)T . The LDA is expected to be a reliable approximation for suﬃciently large systems where ﬁnite-size corrections and gradient terms in the density proﬁle are negligible. It is justiﬁed if the relevant energies are larger than the single-particle excitation energies. The LDA can be applied to a large variety of systems, independent of quantum statistics (bosons and fermions), once one knows the equation of state μ(n, T ). For example, in Chapter 17 it will be applied to strongly interacting Fermi gases.

234

Thermodynamics of a Trapped Bose Gas

For a weakly interacting Bose gas at T = 0, where μ = gn, eqn (13.45) immediately yields the Thomas–Fermi result n(r) = (μ0 − Vext (r))/g for the ground state density, already discussed in the previous chapter. An interesting feature of the local density approximation is the possibility of approaching the problem from a complementary point of view, i.e. that which entails determining the equation of state of complex systems starting from the (experimental) knowledge of the density proﬁles. Recently, this possibility has found a very eﬃcient and rich ﬁeld of applications in both interacting Bose and Fermi gases, at zero as well as at ﬁnite temperatures. The starting point for determining the equation of state from the behaviour of the density proﬁles is provided by a proper integration of the Gibbs–Duhem thermodynamic relation dP = ndμ + sdT,

(13.48)

where P , n, μ, s, and T are the local values of the pressure, density, chemical potential, entropy density, and temperature respectively. Let us consider a trapped conﬁguration at equilibrium where the temperature is uniform. Using the LDA equation (13.45) we can write dμ(n) = d(μ0 − Vext ) = −dVext , where Vext can now be regarded as an integration variable. Integrating eqn (13.48) at a given temperature from the value Vext (x = y = 0, z), where the local pressure of the gas takes the value P = P (x = y = 0, z), up to Vext = ∞ where P = 0, we obtain P (z) ≡ P (x = y = 0, z) =

∞

n[(μ0 − Vext )]dVext .

(13.49)

Vext (x=y=0,z)

In the case of harmonic trapping we can integrate eqn (13.49) in the x–y plane for a ﬁxed value of z, using the diﬀerential relationship dVext = (1/2)md(ωx2 x2 + ωy2 y 2 ), thereby obtaining the useful result (Cheng and Yip, 2007; Ho and Zhou, 2009) P (z) =

mωx ωy n1 (z), 2π

(13.50)

which relates the local pressure to the doubly integrated (also called one-dimensional) density n1 (z) = dxdyn(r). This relation shows that, in the presence of harmonic trapping, we can determine the local pressure at the point (x = 0, y = 0, z) by simply measuring the doubly integrated density. The point (x = 0, y = 0, z) corresponds to a local region of uniform matter with temperature T and chemical potential μ = μ0 − (mωz2 /2)z 2 , so that one can also write

P μ = μ0 −

mωz2 2

2

z ,T =

2 mω⊥ n1 (z, T ). 2π

(13.51)

The previous analysis completes the determination of the equation of state once we know the value of μ0 and T of the trapped gas. Experimentally one possibility is to

Equation of state and density proﬁles

235

explore the behaviour of the measured pressure P (z) for large values of z where the gas behaves classically and to use the expression 2 2

μ/kB T μ0 /kB T −βmωz z = kB T λ−3 e P (z → ∞) = kB T λ−3 T e T e

/2kB T

,

(13.52)

from which we can, in principle, extract the value of T and μ0 . When the temperature is low this method is not very eﬃcient due to the weakness of the signal in the tails of the density, and alternative methods should be found. For example, the temperature can be measured adding another gas in thermal equilibrium behaving like a ‘thermometer’. This approach has been used by Nascimbene et al. (2010b) to determine the equation of state of a dilute Bose gas across the BEC phase transition. If the trapping potential exhibits signiﬁcant anharmonicities, the relationship (13.51) does not hold and in order to determine the local pressure one should rely on the more general equation (13.49), whose implementation requires the actual knowledge of the local density as a function of the external potential. The experimental determination of the local density can be achieved by applying the inverse Abel transform to the measured column density (Shin et al., 2008). This approach only requires that the radial potential is elliptically symmetric, i.e. dependent on the combination αx2 + βy 2 . Alternatively, the local value of the density can be determined from the relation ∂P ∂P n= =− (13.53) ∂μ T Vext T which follows from the Gibbs-Duhem relation (13.48). Once the local density and pressure are known, a third thermodynamic quantity should be determined in order to build the equation of state. In alternative to the measurement of the temperature, which can be problematic at very low temperature, one can measure an other thermodynamic quantity, like the isothermal compressibility ∂n 1 ∂n 1 κT (z) = 2 =− 2 , (13.54) n ∂μ T n ∂Vext T which can be inferred from the gradient of the density. The temperature of the gas can then be extracted a posteriori through the use of thermodynamic relations involving the density, the compressibility, and the pressure. This procedure has been successfully applied to determine the universal thermodynamic functions of the Fermi gas at unitarity (Ku et al., 2012; see also Chapter 16), including the determination of the critical temperature, and of two-dimensional Bose gases (Desbuquois et al., 2014; see also Chapter 23). An important determination of the equation of state, starting from the measurement of the density proﬁles of three-dimensional Bose gases at T 0, was made by Navon et al. (2011). In this case the value of the chemical potential along the z-axis was identiﬁed using the LDA expression μ(z) = μ0 −(m/2)ωz2 z 2 , with μ0 = (m/2)ωz2 Z 2 ﬁxed by the Thomas–Fermi radius Z, where the density vanishes. The Thomas–Fermi radius was measured using an iterated scheme based on ﬁtting procedures of the

236

Thermodynamics of a Trapped Bose Gas

one-dimensional density beyond the mean-ﬁeld prescription (11.7). In this way these authors were able to measure accurately the pressure P of uniform matter as a function of the chemical potential in the form P (μ) = (2 /ma5 )h(ν) where ν = μa3 /g, and to point out the deviations of the equation of state from the mean-ﬁeld value h(ν) = 2πν 2 , caused by the many-body Lee, Huang, and Yang corrections (see Figure 4.2).

13.7

Collective oscillations at a ﬁnite temperature

In Chapter 12 we studied the collective excitations of a trapped Bose gas at zero temperature. In this case, all the atoms are in the condensate and the compressibility of the gas is deﬁned by the mean-ﬁeld interaction between particles; this interaction generates a collective oscillation which is sometimes called Bogoliubov sound. At ﬁnite temperatures the situation is more complicated. On one hand, both the condensate and the thermal cloud can oscillate. On the other hand, collisions between excitations can play an important role and one must distinguish between a collisional and a collisionless regime. Mean-ﬁeld approaches have been used to predict the properties of the collective excitations mainly in the collisionless regime. This regime is achieved at low temperatures and for low densities of the thermal cloud. In this case, the oscillations of the condensate behave similarly to the T = 0 case and can still be called Bogoliubov sound modes. Most of these approaches treat the thermal component as a static thermal bath, and do not account for damping mechanisms. In order to include damping, one actually needs a dynamic description of the oscillations of both the condensate and the thermal cloud. This dynamic coupling can also be important in the determination of the temperature dependence of the frequency shift (see, for example, Giorgini, 2000). At high temperatures and/or high densities, collisions are more important and can aﬀect the nature of the collective excitations. In Bose superﬂuids the collisional regime is described by the equations of two-ﬂuid hydrodynamics and is characterized by the occurrence of two distinct oscillations: ﬁrst and second sound. As discussed in Section 6.6, in a weakly interacting Bose gas ﬁrst sound mainly involves the thermal cloud, except at extremely low temperatures, and reduces to the usual hydrodynamic sound above Tc ; conversely, second sound is essentially the oscillation of the condensate and disappears above Tc . This behaviour diﬀers signiﬁcantly from the case of highly incompressible ﬂuids, like liquid helium or the unitary Fermi gas (see Chapter 19), where second sound is mainly an entropy oscillation and the normal and superﬂuid components move out of phase, the total density remaining practically constant. The propagation of second sound in an elongated Bose gas has been observed by Meppelink et al. (2009), who were able to excite a sound wave in an elongated conﬁguration at a ﬁnite temperature. The hydrodynamic regime was achieved working with a dense sample of sodium atoms. This work has conﬁrmed that the superﬂuid density of a dilute Bose gas practically coincides with the density of the condensate. The discretized oscillations of a trapped Bose gas at ﬁnite temperatures permit an easy description in the hydrodynamic regime. For √ example, the frequency of the quadrupole oscillation is given by the simple expression 2ωho , independent of temperature, and this diﬀers from the collisionless frequency 2ωho , so that the measurement of the

Collective oscillations at a ﬁnite temperature

237

0.3

Im(ω)/ωz

0.2

0.1 ωτ = 0 0 1.5

1.6

ωτ = ∞ 1.7

1.8 Re(ω)/ωz

1.9

2

Figure 13.7 The imaginary part of ω versus its real part for the low m = 0 mode in a cigar trap. The solid line is the interpolation formula (13.55) calculated for ωC = 2ωz and ωH = (12/5)1/2 ωz . The solid circle is the measurement of Stamper-Kurn et al. (1998c). The open circles are the measurements of Leduc et al. (2002).

quadrupole oscillation can be employed as a useful indicator of the achievement of the collisional regime. The transition from the collisionless to the hydrodynamic regimes takes place when ωτ is of order 1, where τ is a typical collision time. A useful interpolation formula between the two regimes is provided by the law 2 ω 2 = ωC +

2 2 ωHD − ωC , 1 + iωτ

(13.55)

predicted by general theory of relaxation √ phenomena (Landau and Lifshitz, 1987a, §81). Here, ωC = 2ωho and ωHD = 2ωho are the frequencies of the quadrupole mode in the collisionless and hydrodynamic regimes, respectively. A peculiar property predicted by eqn (13.55) is the occurrence of an imaginary part in the collective frequency. Damping is maximum in the intermediate regime, where ωτ ∼ 1. The shift of the frequencies in the two regimes and the enhancement of damping represent peculiar features characterizing the transition between the collisionless and the collisional regimes (see Figure 13.7). Evidence for a signiﬁcant damping of the quadrupole oscillation in cigar-type conﬁgurations has been found (Stamper-Kurn et al., 1998c; Leduc et al., 2002), in reasonable agreement with the theory. Let us ﬁnally point out the importance of other nonequilibrium processes which are associated with the exchange of atoms between the condensate and the thermal cloud. A pioneering experiment in this area of study was carried out at MIT by suddenly cooling an atomic cloud below the BEC transition and measuring the time evolution of the condensate fraction (Miesner et al., 1998). The collisional mechanisms at ﬁnite temperatures, in the presence of Bose–Einstein condensation, have been the object of rather extensive theoretical work whose discussion goes beyond the scope of this volume (for a general review see, for example, Griﬃn et al., 2009).

14 Superﬂuidity and Rotation of a Trapped Bose Gas In Chapter 12 we illustrated the dynamic behaviour of trapped Bose–Einstein condensed gases, with special emphasis on the collective excitations. The comparison with experiments has revealed the high accuracy of Gross-Pitaevskii theory which, in the Thomas–Fermi limit, takes the simple form of the hydrodynamic equations of superﬂuids. Though the propagation of sound and the occurrence of collective oscillations are important consequences of the superﬂuid nature of such systems, the emergence of these phenomena cannot be considered a direct proof of superﬂuidity. In fact, the propagation of sound is not a unique peculiarity of the superﬂuid phase. For example, strongly interacting Fermi gases also exhibit a typical hydrodynamic behaviour above the critical temperature (see Chapter 19). This chapter is devoted to discussing important superﬂuid properties exhibited by dilute Bose gases conﬁned in external traps. A ﬁrst key issue concerns the absence of viscosity and the applicability of Landau’s criterion for superﬂuidity (Section 14.1). The absence of viscosity signiﬁcantly changes the rotational properties of the gas, as we will discuss in the following sections. Sections 14.2 and 14.3 focus on the changes in the moment of inertia caused by the irrotationality of the superﬂuid motion at small angular velocities and on their consequences on the scissors mode. The expansion of a rotating superﬂuid cloud is discussed in Section 14.4, while the stability of the rotating conﬁgurations is the object of Section 14.5. At high angular velocities rotational eﬀects are characterized by the appearance of quantized vortices and vortex lattice structures (Section 14.6). The stable existence of these vortices is actually a direct proof of superﬂuidity. Measurable consequences of the presence of vortices on the collective oscillations of the trapped gas are discussed in Section 14.7, while the stability and precession of vortex lines are the topics of Section 14.8. Finally, in Section 14.9, we discuss the nature of the superﬂuid ﬂow in toroidal traps.

14.1

Critical velocity of a superﬂuid

Superﬂuidity in uniform systems is associated with the existence of a critical velocity, ﬁxed by the spectrum of elementary excitations. Below the critical velocity vc = min (p)/p a moving heavy impurity or a moving boundary cannot create excitations without violating energy and momentum conservation (Landau criterion, see Section 6.1). The existence of a critical velocity is deeply connected with the presence

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Critical velocity of a superﬂuid

239

Energy transfer rate [nk/s]

of interactions, which make the compressibility of the system ﬁnite, as well as with the irrotationality constraint which rules out the existence of low-energy excitations of transverse nature. With careful choices of the geometry of the conﬁning potential and of the external perturbation such critical eﬀects can also be explored in trapped Bose gases. Critical velocities in Bose–Einstein condensates were ﬁrst studied experimentally by moving a focused laser beam through the condensate (Raman et al., 1999; Onofrio et al., 2000). If the velocity of the ‘moving impurity’ exceeds a critical value strong dissipative eﬀects are observed through ﬁnal temperature measurements (Figure 14.1). The nature of the excitations created in such experiments cannot however be easily identiﬁed. The practical implementation of Landau’s criterion is not simple. For example, it is well known that in the case of superﬂuid helium the application of this criterion to the phonon–roton branch of the excitations (see Figure 8.2) gives too large values of vc . This contradiction was explained by Feynman (1954) who suggested that the dissipation in the ﬂuid could be related to creation of vortex rings whose dispersion is given by eqn (5.35). The critical velocity associated with the creation of a ring of radius 0 R0 is vc = mR ln 1.59R and consequently can in principle be arbitrary small. The ξ 0 actual critical velocity is ﬁnite because the probability of the creation of a vortex ring of large radius can be very small or precluded by the geometry of the problem. This means that the critical velocity depends on the actual conditions of the experiment. A general problem concerns the ﬂow of the superﬂuid around an obstacle. The latter can be a laser beam moving with respect to the ﬂuid, or a potential barrier generating

300

200

100

0 0

1 2 3 Stirring velocity [mm/s]

4

Figure 14.1 Evidence for critical velocity in a trapped condensate. The energy transfer rate, obtained from temperature measurements, is shown as a function of the stirring velocity of a moving focused laser beam. If the velocity of the moving ‘impurity’ is small no dissipative eﬀects are observed. From Onofrio et al. (2000). Reprinted with permission from Physical c 2000, American Physical Society. Review Letters, 85, 2228;

240

Superﬂuidity and Rotation of a Trapped Bose Gas

a constriction in a toroidal trap (see Section 14.10). If the obstacle is macroscopic, i.e. if its size is larger than the healing length, the critical velocity can be calculated using the hydrodynamic equations (6.17) and (6.19), which are the Euler equations of the potential motion of a ﬂuid without dissipation. An important property of a stationary ﬂow is that the velocity near the obstacle is larger than that at large distances. Furthermore, the local sound velocity is smaller than that at larger distances because of the smaller value of the density. It then follows that the critical velocity, ﬁxed by the condition that the velocity of the ﬂuid will reach the local sound velocity at some point near the obstacle, can be signiﬁcantly smaller than the value of the sound velocity far from the obstacle. For larger velocities the region near the obstacle will be characterized by a supersonic ﬂow. The Euler equations cannot describe in a continuous way the transition between the subsonic and the supersonic region (see, for example, Landau and Lifshitz, 1987a, Section 122). In the case of a normal ﬂuid the supersonic region is characterized by a jump of the density, causing the creation of shock waves and dissipative eﬀects. In a superﬂuid, instead, quantized vortex lines (Frisch, Pomeau, and Rica, 1992) or solitons will be created. The quantitative description of these objects requires the explicit inclusion of quantum eﬀects, like the quantum pressure. In a dilute BEC it can be performed using the GP equation. The ﬁrst experiments revealing the creation of solitons produced by fast-moving potential barriers applied to an elongated condensate were carried out by Engels and Atherton (2007). The critical velocity caused by the presence of a macroscopic obstacle can easily be calculated in one dimension (Hakim, 1997; Leboeuf and Pavloﬀ, 2001). Let us consider a Bose–Einstein condensate moving in a stationary way along the z-direction through a potential barrier Vext (z), satisfying the conditions for the applicability of the local density approximation. For a stationary motion the current j = n(z)v(z) = n∞ v∞ does not depend on z and is hence ﬁxed by the asymptotic values of the density n∞ and of the velocity v∞ at large distances, where Vext → 0. The Bernoulli equation, which ﬁxes the constancy of the chemical potential in the presence of ﬂow, then takes the form m

2 v2 mv∞ + μ (n) + Vext (z) = + mc2∞ . 2 2

(14.1)

By deﬁnition, the condition of criticality v∞ = vcr for the ﬂow corresponds to a point inside the barrier where the condition v(z) = c(z) is satisﬁed. It is not diﬃcult to show that this condition will be achieved at the point z = zmax , where the external potential has a maximum Vmax . Taking into account that the current is z-independent and that for a BEC gas n(z) = mc2 (z)/g, we ﬁnd that the sound velocity at zmax is given by c3 (zmax ) = gn∞ vcr /m = vcr c2∞ . Substitution of this relation into (14.1) gives a simple algebraic equation for vcr (Watanabe et al., 2009): 2 2/3 mvcr 3 m vcr c2∞ = mc2∞ − Vmax . − 2 2

(14.2)

In more complicated geometries the problem can only be solved numerically. The emission of vortex pairs by the ﬂow around a hard disc in a uniform two-dimensional Bose–Einstein condensate was investigated theoretically by

Moment of inertia

241

Frisch et al. (1992). These authors solved numerically the two-dimensional-GP equation with the boundary condition Ψ = 0 on the boundary of the disc. They discovered that when the velocity of the ﬂow exceeds the critical value vc ≈ 0.4c the emission of vortex pairs begins, resulting in a drag force on the disc. The creation of vortex pairs caused by a moving obstacle was investigated experimentally in three dimensions by Neely et al. (2010). The condensate had the ‘pancake’ shape and was pierced by a laser beam of radius 10μm serving as a repulsive obstacle of macroscopic size as compared to the healing length. The ﬂow was created by translating the trap at a constant velocity. The authors observed the emission of vortex dipoles at v > vc ∼ 0.1c, where c is the sound velocity in the centre of the trap. The experiment was successfully simulated by the numerical solution of the three-dimensional GP equation. As already pointed out in Section 6.1, in Galilean invariant systems the Landau criterion for superﬂuidity is directly related to the stability of persistent currents. Persistent currents in a trapped superﬂuid gas can be generated by creating vortices. A particularly convenient geometry is provided by toroidal conﬁgurations (Ryu et al., 2007) whose key properties will be discussed in Section 14.9. These conﬁgurations are well suited to investigating, in particular, the dissipation of energy of the superﬂuid ﬂow through thin capillaries. It was suggested by Anderson (1966) that the dissipation of a superﬂuid through a thin capillary is connected with the occurrence of ‘phase slips’. The slip occurs when a vortex line crosses the cross-section of the capillary. Then the phase of the order parameter undergoes a jump ΔS = 2π. This picture was conﬁrmed in a series of important experiments carried out in superﬂuid Helium (Avenel and Varoquaux, 1985; Simmonds et al., 2000). Some key features of phase slips in dilute Bose–Einstein condensed gases will be discussed in Section 14.9 in the context of toroidal conﬁgurations. The following sections are devoted to discussing superﬂuid phenomena exhibited by rotating Bose–Einstein condensed gases. These include, among others, the quenching of the moment of inertia due to irrotationality and the occurrence of quantized vortices. For more systematic discussions on rotating Bose–Einstein condensates, see the review article by Fetter (2009). Other superﬂuid phenomena, like Josephson-type eﬀects, will be discussed in the next Chapter.

14.2

Moment of inertia

The moment of inertia Θ relative to the z-axis can be deﬁned as the response of the system to a rotational ﬁeld Hpert = −ΩLz according to the relationship

Lz = ΩΘ,

(14.3)

where Lz = i (xi pyi − yi pxi ) is the third component of angular momentum and the average is taken on the stationary conﬁguration in the presence of the perturbation. For a classical system the moment of inertia takes the rigid value 2 Θrig = N mr⊥ ,

(14.4)

2 and can be simply evaluated in terms of the radial square radius r⊥ ≡ x2 + y 2 . In contrast, the quantum determination of Θ is much less trivial. In the limit of small

242

Superﬂuidity and Rotation of a Trapped Bose Gas

angular velocities Ω one can employ the formalism of linear response (Chapter 7). In this case the moment of inertia can be expressed as Θ = 2Q−1

n,m

e−βEm

|n|Lz |m|2 , En − Em

(14.5)

where |n and En are eigenstates and eigenvalues of the unperturbed Hamiltonian and Q is the partition function. A natural way to evaluate the moment of inertia is to rotate the conﬁning trap with angular velocity Ω and to look for the consequent stationary solutions in the rotating frame. The corresponding expectation value Lz then permits us to evaluate the moment of inertia through deﬁnition (14.3). A similar procedure can also be implemented experimentally to generate the rotation of the system: one rotates the trap and waits for the system to be in thermal equilibrium in the rotating frame. In order to ensure thermalization the trap should not be perfectly symmetric in the plane of rotation, otherwise no angular momentum can be transferred to the system. The rotating apparatus exhibits an important resemblance to the rotating bucket experiment of liquid helium (Chapter 8). In the case of helium the possibility of transferring angular momentum is ensured by the microscopic roughness of the container. Conversely, the roughness of the rotating potential which traps atomic gases has a more ‘macroscopic’ nature and is realized experimentally by adding a small deformation to the conﬁning potential. The equations of motion in the frame rotating with the trap are easily obtained by adding the term −ΩLz to the Hamiltonian, where Ω is the angular velocity of the rotating trap. In the case of a dilute Bose gas at zero temperature the Gross-Pitaevskii equation takes the form ∂ 2 2 i Ψ = − ∇ + Vext + g|Ψ0 |2 + iΩr × ∇ Ψ . (14.6) ∂t 2m Since in this equation r is the coordinate in the rotating frame, the trapping potential Vext no longer depends on time. Actually, only in this frame, does it make sense to look for stationary solutions in the presence of a deformed rotating trap. In the laboratory frame such solutions correspond to a steady rotation of the condensate with angular velocity Ω. In the Thomas–Fermi limit, the Gross-Pitaevskii equation reduces to the hydrodynamic equations of superﬂuids (see Section 5.2) which, in the rotating frame, take the form ∂n + ∇ · (n(v − Ω × r)) = 0 ∂t and ∂v +∇ ∂t

v2 Vext g + + n − v · (Ω × r) 2 m m

(14.7) = 0.

(14.8)

The above equations show that the rotation aﬀects both the equation of continuity and the Euler equation. Here v = (/m)∇S, where S is the phase of the order

Moment of inertia

243

parameter, is the superﬂuid velocity in the laboratory frame, expressed in terms of the coordinates of the rotating frame. It obeys the usual irrotationality constraint. In the presence of harmonic trapping Vext (r) = (m/2) ωx2 x2 + ωy2 y 2 + ωz2 z 2 , an interesting class of stationary solutions of the hydrodynamic equations is obtained by making the irrotational ansatz v = α∇(xy).

(14.9)

The equilibrium density, derivable from eqn (14.8) by setting ∂v/∂t = 0, still has the form of an inverted parabola, while the equation of continuity permits us to derive the useful relationship α = −δΩ,

(14.10)

where δ=

y 2 − x2 y 2 + x2

(14.11)

is the deformation of the atomic cloud in the x–y plane. By calculating the angular momentum corresponding to the velocity ﬁeld (14.9) one ﬁnds that the moment of inertia is given by the irrotational form Θ = δ 2 Θrig .

(14.12)

Notice that the above results do not assume small angular velocity and that in general the value of δ will depend on Ω (see Section 14.5). In this section we restrict the discussion to the linear regime of small angular velocities, where the deformation parameter (14.11) can be evaluated at rest and coincides with the deformation of the trap: =

ωx2 − ωy2 . ωx2 + ωy2

(14.13)

Equations (14.11) and (14.12) have been obtained by solving the equations of motion in the Thomas–Fermi limit. The same result also holds in the noninteracting limit where, however, the relationship between the deformation parameter δ and the oscillator frequencies has the diﬀerent form δ = (ωx − ωy )/(ωx + ωy ). This dependence originates from the diﬀerent scaling exhibited by the condensate density in terms of the trapping frequencies (see eqn (10.43)). Equations (14.11) and (14.12) reveal the crucial eﬀect played by superﬂuidity which, as a consequence of the irrotationality constraint, implies a reduced capability for the system to carry angular momentum. The above results were derived at zero temperature where the whole system is superﬂuid. Above the critical temperature for BEC the system becomes normal and it is consequently important to discuss the temperature dependence of the moment of inertia. This can be calculated in an exact way in the noninteracting model, where a

244

Superﬂuidity and Rotation of a Trapped Bose Gas

fully analytical solution is available in the presence of harmonic trapping. In this case the calculation of Θ can be obtained through the algebraic solution of the equation ˆ X] ˆ =L ˆz [H,

(14.14)

ˆ the knowledge of which permits us to write the moment of inertia for the operator X, ˆ z , X]. ˆ Using the harmonic oscillator Hamiltonian for H one ﬁnds in the form Θ = [L the analytic solution X = −(i/) i [(ωx2 + ωy2 )xi yi + 2pxi pyi /m]/(ωx2 − ωy2 ) and the moment of inertia takes the form Θ=

! mN (y 2 − x2 )(ωx2 + ωy2 ) + 2(ωy2 y 2 − ωx2 x2 ) , ωx2 − ωy2

(14.15)

where we have used the virial identities p2x = m2 ωx2 x2 and p2y = m2 ωy2 y 2 . Equation (14.15) is meaningful only if ωx = ωy . However, it admits a well-deﬁned limit when ωx → ωy . In the calculation of the square radii x2 and y 2 it is useful to separate the contribution arising from the condensate, which in the noninteracting model scales like ωx−1 and ωy−1 , from that of the thermal component. The latter is easily evaluated in the semiclassical approximation kB T ωx , ωy , ωz , where x2 T and y 2 T scale like ωx−2 and ωy−2 , respectively. One ﬁnally ﬁnds the result (Stringari, 1996a) 2 2 δ 2 r⊥ 0N0 + r⊥ T(N − N0 ) Θ = 2 2 Θrig r⊥ 0N0 + r⊥ T(N − N0 )

(14.16)

for the ratio between the moment of inertia and its rigid value (14.4), where the averages 0 and T refer to the condensate and thermal components, respectively. Result (14.16) explicitly shows that above Tc , where N0 /N = 0, the moment of inertia takes the rigid value, while at T = 0 it reduces to the irrotational form (14.12). It is worth discussing the behaviour of the moment of inertia in the thermodynamic limit 3 2 2 N → ∞, where N ωho is kept constant. In this limit, the ratio r⊥ 0 /r⊥ T tends to zero and one ﬁnds Θ/Θrig → 1 everywhere except at T 0, where N0 N. This behaviour is not surprising. In fact, if the radius of the condensate is much smaller than the one of the thermal component then there is no distinction between Θ and Θrig since in both cases the leading contribution is given by the thermal component. For ﬁnite values of N the ratio Θ/Θrig tends smoothly to zero as the temperature decreases. An example is shown in Figure 14.2 for a spherical trap and two diﬀerent values of N . Result (14.16) is also expected to be valid in the presence of interactions to the extent that the relevant excitations which contribute to thermodynamics are well described by the single-particle picture (see Section 13.2) and the condensate can be identiﬁed with the superﬂuid component. This is a good approximation for a weakly interacting gas except at very low temperatures and close to the critical temperature, where the superﬂuid component must be distinguished from the condensate. Actually, under this approximation, eqn (14.16) exactly reduces to the superﬂuid formula 2 Θ = m dr⊥ r⊥ (n − ns ) (14.17)

Scissors mode

245

1

0.8

Θ/Θrig

0.6

0.4

0.2

0

0

0.2

0.4

0.6

0.8

1

T/Tc

Figure 14.2 Moment of inertia Θ divided by the rigid value Θrig as a function of T /Tc . The solid line corresponds to the interacting gas in the thermodynamic limit with η = 0.4. The dotted and dashed lines are the predictions for 5 × 107 and 5 × 104 noninteracting particles, respectively, in a spherical trap.

for the moment of inertia, here written for a cylindrically symmetric conﬁguration, where ns (r) is the superﬂuid density. Interactions can aﬀect the ratio (14.16) by changing the temperature dependence of the condensate density. The change is particularly signiﬁcant at large N . 2 2 In fact, unlike in the noninteracting case, the ratio r⊥ 0 /r⊥ T does not vanish in the thermodynamic limit and is ﬁxed by the value of the scaling parameter η (see Section 13.1). As a consequence, interactions have the important eﬀect of reducing the value of the moment of inertia with respect to the rigid value in the whole range of temperatures below Tc . This behaviour is explicitly shown by the solid line in Figure 14.2.

14.3

Scissors mode

In trapped gases the direct measurement of the moment of inertia through deﬁnition (14.3) is diﬃcult because the detection of angular momentum is not easy in these dilute samples. In a deformed trap, however, angular momentum is coupled with the quadrupole degrees of freedom and consequently, by measuring the shape oscillations of the rotating conﬁguration, one can obtain useful information on the angular momentum and hence on the moment of inertia. This is well illustrated by the exact commutation rule between the Hamiltonian and the angular momentum operators: [H, Lz ] = im(ωy2 − ωx2 )

i

xi y i .

(14.18)

246

Superﬂuidity and Rotation of a Trapped Bose Gas

An instructive example of such a coupling is provided by the so-called scissors mode, an oscillation of the gas caused by the sudden rotation of a deformed trap. As a consequence of the rotation the gas will no longer be in equilibrium and will start oscillating around the new equilibrium position. If the angle of rotation φ0 of the trap is small compared to the deformation (14.13), the rotation of the harmonic potential will produce the perturbation δVext = (ωx2 − ωy2 )φ0 xy, which naturally excites the quadrupole mode. The behaviour of the resulting oscillation depends in a crucial way on whether the system is normal or superﬂuid. In fact, while the restoring force associated with the motion is in both cases quadratic in the deformation parameter (14.13), the mass parameter, being proportional to the moment of inertia, behaves quite diﬀerently in the two cases. The ﬁnal result is that a nonsuperﬂuid gas, characterized by the rigid value for the moment of inertia, will exhibit an oscillation with vanishing frequency as → 0. In contrast, no low-frequency mode can occur in a superﬂuid. By solving the hydrodynamic equations in the laboratory frame with the ansatz δn ∝ xy and v ∝ ∇(xy), one easily ﬁnds that the small-amplitude oscillation of the condensate corresponds to a rotation whose angle oscillates around the new equilibrium value with frequency (Gu´ery-Odelin and Stringari, 1999) # ωHD = ωx2 + ωy2 . (14.19) The experiments on the scissors mode carried out for T Tc (Marag`o et al., 2000) have conﬁrmed with high precision the predictions of theory (see Figure 14.3). Unlike the superﬂuid, the normal gas in the collisionless regime instead exhibits two frequencies occurring at ω± = |ωx ± ωy |. In particular, the low-frequency solution |ωx − ωy | is characterized by crucial rotational components in the velocity ﬁeld which are absent 8 theory Oxford exp. 4

φ [º]

0 −4 −8 −12

5

10

15

20 Time [ms]

25

30

35

Figure 14.3 The time evolution of the scissors-mode oscillation for a Bose–Einstein condensed gas. The measured oscillating frequency agrees very well with the predicted value obtained from eqn (14.19). From Marag` o et al. (2000). Reprinted with permission from c 2000, American Physical Society. Physical Review Letters, 84, 2056;

Expanding a rotating condensate

247

8 theory Oxford exp.

4

φ [º]

0 −4 −8 −12

5

10

15

20 Time [ms]

25

30

35

Figure 14.4 The time evolution of the scissors-mode oscillation for a thermal cloud above Tc . In this case the oscillation of the scissors mode, in the absence of collisions, is characterized by the two frequencies |ωx ±ωy |. The agreement between theory and experiment is very good. From Marag` o et al. (2000). Reprinted with permission from Physical Review Letters, 84, 2056; c 2000, American Physical Society.

in the superﬂuid motion. Also, in this case the agreement between theory and the experiments carried out above Tc is very good (see Figure 14.4).

14.4

Expanding a rotating condensate

Another important consequence of irrotationality concerns the expansion of a rotating gas. In Section 12.7 we have shown that after releasing the trap the gas expands fast in the tight direction and soon reaches a symmetric shape (δ = 0) in the x–y plane. At larger times the expansion continues, producing a change of sign in the value of the deformation. If a deformed gas is initially rotating with angular velocity Ω0 the expansion proceeds in a diﬀerent way. In fact, in this case the deformation of the gas cannot reach the value δ = 0 because this would result in a violation of angular momentum conservation. Due to the irrotationality constraint of the superﬂuid motion no angular momentum can indeed be carried by a symmetric (δ = 0) conﬁguration. Actually, the angular velocity Ω will increase rapidly as δ → 0, but because of energy conservation there will necessarily be a maximum value of Ω, and hence a minimum value of |δ|, that cannot be overcome. These values are easily estimated if one assumes that the rotational energy of the gas, at the time tcr of highest angular velocity, is of the order of the initial energy E0 of the sample. By using the conservation laws Ω0 Θ0 = Ωcr Θcr and E0 Ω2cr Θcr /2 one ﬁnds Θcr Ω20 Θ20 /E0 and Ωcr E0 /(Ω0 Θ0 ), where Ω0 and Ωcr are, respectively, the values of the angular velocity at t = 0 and t = tcr . Since the moment of inertia of a superﬂuid behaves like the square of the deformation parameter (see eqn (14.12)), the minimum deformation turns out to be linear in the initial angular velocity Ω0 , while the critical frequency Ωcr behaves as the inverse

248

Superﬂuidity and Rotation of a Trapped Bose Gas 1.7 1.6 1.5

Aspect ratio

1.4 1.3 1.2 1.1 1.0 0.9 0.8 0

2

4

6

8

10

12

14

16

18

20

Time [ms]

Figure 14.5 The aspect ratio of a condensate in time of ﬂight. Initially rotating condensates (upper and middle curves) exhibit a strong backbending eﬀect and never become circular. After release from a noninteracting trap, the aspect ratio instead decreases steadily (lower curve). The curves correspond to the theory of Edwards et al. (2002). Experimental points are from Hechenblaikner et al. (2002). Reprinted with permission from Physical Review Letters, c 2002, American Physical Society. 88, 070406;

of Ω0 . These qualitative arguments are conﬁrmed by the numerical solution of the equations of motion which is easily available using the Thomas–Fermi approximation (Edwards et al., 2002). This peculiar behaviour exhibited by the expansion of a rotating superﬂuid has been conﬁrmed experimentally with good accuracy by Hechenblaikner et al. (2002) (see Figure 14.5).

14.5

Rotation at higher angular velocities

In Section 14.2 we have discussed the stationary solution of the hydrodynamic eqns (14.6)–(14.8) in the linear regime of small angular velocities. It is interesting to discuss how the system behaves at higher Ω, where nonlinear eﬀects play a crucial role in the solution of the hydrodynamic equations. As already pointed out, in the presence of a rotating trap one can obtain stationary solutions using the ansatz v = α∇(xy) of eqn (14.9). The value of α is directly related to the deformation of the condensate and to the angular velocity by the relation α = −δΩ (see eqn (14.10)). By substituting (14.9) into eqn (14.8) one immediately ﬁnds that the equilibrium density is given by the parabolic shape n(r) =

1 m μ ˜ − (˜ ω x x2 + ω ˜ y y2 + ω ˜z z2 ) g 2

(14.20)

Rotation at higher angular velocities

249

also in the presence of the rotation. This equation deﬁnes the density in the region where n ≥ 0. Elsewhere one has n = 0. The new distribution is characterized by the renormalized oscillator frequencies ω ˜ x2 = ωx2 + α2 − 2αΩ,

(14.21)

ω ˜ y2 = ωy2 + α2 + 2αΩ.

(14.22)

The rotation of the trap, providing a value of α diﬀerent from zero, has the consequence of modifying the shape of the density proﬁle, through the change of the eﬀective frequencies. In particular, the deformation of the atomic cloud takes the form δ=

ω ˜ x2 − ω ˜ y2 , ω ˜ x2 − ω ˜ y2

(14.23)

which approaches the static value δ = when Ω and α → 0. By using the relationship α = δΩ one then ﬁnds the following third-order equation for α (Recati et al., 2001): 2 2 α3 + α ω⊥ − 2Ω2 + Ωω⊥ = 0, (14.24) 2 = (ωx2 + ωy2 )/2. Depending on the value of Ω and of the dewhere we have deﬁned ω⊥ formation of the trap one can ﬁnd diﬀerent regimes, but only the solutions satisfying the conditions of normalizability ω ˜ x2 > 0, ω ˜ y2 > 0 should be retained. For an √ axisymmetric trap ( = 0) the solutions have a very simple structure. For Ω < ω⊥ / 2 only ﬂuid. √ the solution α = 0 is available, corresponding to a nonrotating 2, For Ω > ω⊥ / 2 the equation exhibits a new class of solutions α = ± 2Ω2 − ω⊥ corresponding to a spontaneous breaking of the axial rotational symmetry (δ = 0). This is the analogue of the bifurcation from the axisymmetric Maclaurin to the triaxial Jacobi ellipsoids for rotating classical ﬂuids. As a consequence of this behaviour, the system can take a deformed shape even if the rotating trap is symmetric or almost symmetric in the x–y plane. The physical origin of this eﬀect can be simply understood in terms of the energetic instability of the quadrupole mode m = +2, whose energy, in √ the laboratory frame, is given by ωm=+2 = 2ω⊥ (see eqn (12.13)). In the rotating frame √ the energy of this mode, which carries two √ units of angular momentum, is ( 2ω⊥ − 2Ω) and becomes negative for Ω > ω⊥ / 2. If = 0 the solutions are no longer symmetric under the change α → −α. Even small values of change the solutions of eqn (14.24) in a signiﬁcant way. For = 0 eqn (14.24) predicts the occurrence of two branches (see Figure 14.6). The ﬁrst one (normal branch) starts at Ω = 0 and ends at Ω = ωy (we assume here ≥ 0, i.e. ωy < ωx ). The deformation of the cloud in this branch has the same sign as the one of the trap and approaches the value δ = for Ω → 0. The second branch, hereafter called overcritical, starts at inﬁnity, exhibits a backbending, and ends at Ω = ωx . The deformation of the atomic cloud in the overcritical branch is opposite to the one of the trap (δ < 0). It is worth noticing that if ≥ 0.2 the backbending of the overcritical branch takes place for Ω larger than ωy . As a consequence, in this case there is a window of angular velocities where eqn (14.24) has no solutions satisfying the conditions ω ˜ x2 > 0, ω ˜ y2 > 0.

250

Superﬂuidity and Rotation of a Trapped Bose Gas

ε = 0.02

α/ωx

1

0

−1

0

0.5

1 Ω/ωx

Figure 14.6 Stationary solutions of eqn (14.24) as a function of the angular velocity Ω of the trap for = 0.02. The dashed lines are the stationary solutions of the noninteracting Bose gas. The dotted straight lines correspond to Ω = ωy and Ω = ωx .

The solutions of (14.24) diﬀer in a signiﬁcant way from the predictions of the ideal Bose gas (dashed line in Figure 14.6). Actually, the breaking of axial rotational symmetry is the result of two-body interactions and is absent in the noninteracting case. Another important diﬀerence is that the ideal Bose gas has no stationary solution in the interval ωy < Ω < ωx . An important question to discuss is the stability of the above solutions. In fact, at large angular velocities they do not correspond to the ground state of the system. For example, quantized vortices become energetically favourable at some critical value of Ω (see next section). In general one should distinguish between energetic and dynamic instability. The former corresponds to the absence of thermodynamic equilibrium and its signature, at zero temperature, is given by the occurrence of excitations with negative energy. The latter is instead associated with the decay of the initial conﬁguration and is revealed by the existence of excitations with a complex frequency. Let us ﬁrst discuss the stability with respect to the motion of the centre of mass. In the presence of harmonic trapping the equations of motion, in the rotating frame, take the classical form x ¨ = −(ωx2 − Ω2 )x − 2Ωy, ˙

(14.25)

y¨ = −(ωy2 − Ω2 )x + 2Ωx, ˙

(14.26)

z¨ = −ωz2 z,

(14.27)

where x, y, and z are the coordinates of the centre of mass. The eﬀect of the rotation couples the motion in the x and y directions due to the Coriolis force. It can now be found that the solutions of these equations obey the dispersion law # 1 2 ωx + ωy2 + 2Ω2 ± (ωx2 − ωy2 )2 + 8Ω2 (ωx2 + ωy2 ) ω2 = (14.28) 2

Rotation at higher angular velocities

251

and are dynamically stable (ω 2 > 0) for both Ω < ωy and Ω > ωx . In contrast, in the window ωy < Ω < ωx the motion of the centre of mass is dynamically unstable, its position growing exponentially in time. The conditions of stability for the other excitations require careful investigation. It turns out that the normal branch is dynamically stable against quadrupole oscillations (Recati et al., 2001), but at some point it exhibits a dynamic instability against the appearance of oscillations of higher multipolarity (Sinha and Castin, 2001). Concerning the overcritical branch, one instead ﬁnds that the part of the branch with dα/dΩ > 0 is dynamically unstable while the

(a) (I)

0.6

( II )

|~ α|

0.4

0.2

0 (b)

Lz/ħ

6 4 2 0 0.5

0.6

0.7

0.8 ~ Ω

0.9

1.0

Figure 14.7 The measured value of |α| ˜ = |α/ω⊥ | as a function of the stirring frequency ˜ = Ω/ω⊥ is shown in (a). The results of the ascending ramp are shown by solid circles and Ω the ones of the descending ramp by empty circles. The solid lines are the theoretical curves calculated with = 0.022. The normal (I) and overcritical (II) branches are shown. The dashed and dotted lines are solutions of (14.24) at = 0. In (b) the measure of the angular momentum per particle in units of reveals the presence of vortices for the ascending ramp ˜ = 0.75. From Madison et al. (2001). Reprinted with permission from Physical Review above Ω c 2001, American Physical Society. Letters, 86, 4443;

252

Superﬂuidity and Rotation of a Trapped Bose Gas

remaining part is always stable except in a very narrow interval of angular velocities corresponding, in traps with ∼ 0 and ωz ω⊥ , to √ an accidental degeneracy between the m = −2 quadrupole mode with frequency 2ω⊥ + 2Ω and the low m = 0 oscillation with frequency 5/2ωz . Quite remarkably, in the window ωy < Ω < ωx the quadrupole oscillation is dynamically stable if is suﬃciently small. Thus one has the counter-intuitive situation that in this window the repulsive interactions not only generate a stationary solution which was absent in the ideal case, but also ensure full stability to the internal oscillations of the condensate. In the experiment of Madison et al. (2001) the normal branch was realized by ramping up adiabatically the angular velocity to Ω ∼ 0.75ω⊥ . For larger angular velocities this branch exhibits dynamic instability, resulting in the nucleation of vortices (see Figure 14.7). In the same experiment the overcritical branch has also been explored starting from high angular velocities. In this case one can follow the branch down to a critical value below which the system jumps into the normal branch. Also, the stability of the internal shape of the condensate in the interval ωy < Ω < ωx has been veriﬁed directly, while the motion of the centre of mass has been explicitly shown to be unstable in the same interval (Rosenbusch et al., 2002).

14.6

Quantized vortices

The discussion of quantized vortices in trapped atomic gases is of great importance because their study provides a unique test of the theory of interacting inhomogeneous Bose gases at distances of the order or smaller than the healing length. In fact, almost all the quantities discussed so far test the Gross-Pitaevskii theory at a more macroscopic level, where the relevant distances are larger than the healing length. The theory of vortices in a trapped Bose gas consists of a natural generalization of the formalism developed in Section 5.3 in which one takes into account the new geometry of the problem. This has important consequences on the structure of vortices, on their stability and dynamical behaviour. Let us consider the simplest case of an axially symmetric trap and look for vortical solutions of the GP equation in the form Ψ0 (r) = Ψv (r⊥ , z) exp(iϕ),

(14.29) where ϕ is the angle around the z-axis, and Ψv (r⊥ , z) = n(r⊥ , z) is a real function. The velocity ﬁeld associated with the vortical conﬁguration has the same structure as for the uniform case, namely v=

, mr⊥

and is characterized by one quantum of circulation according to the law 2π . v · dl = m The angular momentum per particle z ≡

m Lz = N N

(14.30)

(14.31)

dr(r × v)z n(r)

(14.32)

Quantized vortices

253

is exactly equal to . Notice, however, that if the vortex is displaced from the centre then the angular momentum takes a lower value (see Section 14.8). In this case the axial symmetry of the problem is lost and the order parameter cannot be written in the simple form (14.29). The equation for the modulus of the order parameter takes the form

2 2 ∇ 2 m 2 2 2 2 2 − + (ω + r + ω z ) + gΨ (r , z) Ψv (r⊥ , z) = μΨv (r⊥ , z). z v ⊥ 2 2m 2mr⊥ 2 ⊥ ⊥ (14.33) Due to the presence of the centrifugal term, the solution of this equation must vanish on the z-axis. An example is shown in Figure 14.8 where the solid line represents the condensate wave function, Ψv (x, 0, 0). In the inset, we give the contour plot for the density in the x–z plane, n(x, 0, z) = |Ψv (x, 0, z)|2 .

0.3 4 2 z 0 0.2 Wave function

–2 –4 –4

–2

0 x

2

4

0.1

0

0

1

2

3 x [aho]

4

5

6

Figure 14.8 Condensate with a quantized vortex along the z-axis. The order parameter Ψv (x, 0, 0) is plotted in the case of 104 rubidium atoms conﬁned in a spherical trap with aho = 0.79 μm. The solid line is the solution of the stationary GP eqn (14.33). The dot– dash line is the solution of the GP equation in the absence of the vortex. The dashed line 2 is the noninteracting vortex solution Ψv ∝ r⊥ exp[−(m/2)(ω⊥ r⊥ + ωz z 2 )]. All of the wave functions in the ﬁgure are normalized to 1. The inset shows the contour plot for the density in the x–z plane.

254

Superﬂuidity and Rotation of a Trapped Bose Gas

The structure of the core of the vortex is ﬁxed by the balance between the kinetic energy and the two-body interaction term. For a uniform Bose gas, the size of the core is of the order of the healing length ξ = (8πna)−1/2 , where n is the density of the system. For the trapped gas, an estimate of the core size can be obtained using for n the central value of the density in the absence of vortices. The ratio between ξ and the radius R of the condensate takes the form ξ/R = (aho /R)2 (see eqn (11.15)). For the condensate in the ﬁgure, the radius is about 4.1 in units of aho and the ratio ξ/R is then ∼ 0.06. The actual core size also depends, obviously, on the position on the z-axis and becomes larger when the vortex line reaches the outer part of the condensate, where the density decreases. The solution of the Gross-Pitaevskii eqn (14.33) can be used to calculate the energy of the vortex. We will write the energy in the presence of the vortex in the form E = E0 + Ev , where E0 is the ground state energy. The quantity Ev plays a crucial role in determining the criterion of stability for a vortex line in a frame rotating with angular velocity Ω. In fact, in such a frame the Hamiltonian takes the form H = H0 − ΩLz (see eqn (5.33)) and consequently a vortex with one quantum of circulation will become energetically stable for angular velocities larger that the critical value Ωcr =

Ev . N

(14.34)

For angular velocities smaller than Ωcr the ground state without the vortex is instead energetically favourable with respect to the vortical state. The value of the critical angular velocity was derived in Section 5.3 for a uniform gas. Using a local density approximation it is also possible to extend those results to the case of harmonic trapping. In the large-N limit, where the size of the condensate is much larger than the healing length, the density proﬁle is very smooth, so that for each value of z one can solve the Gross-Pitaevskii equation in the x–y plane and integrate over z at the end. For r⊥ R⊥ (z), where R⊥ (z) = R⊥ 1 − z 2 /Z 2 is the condensate size in the radial plane at position z, one can treat the system as a uniform gas and use the solution Ψv =

n(0, z)f

r⊥ , ξz

(14.35)

where z2 r2 n0 (r⊥ , z) = n0 1 − 2 − ⊥2 Z R⊥

(14.36)

is the Thomas–Fermi density proﬁle of the trapped gas in the absence of the vortex and f (x) is the universal function characterizing the vortex solution of the GrossPitaevskii equation in uniform media (see Section 5.3 and Figure 5.2). The function f (x) approaches unity for large x. The radial distance r⊥ enters eqn (14.35) in units of the healing length ξz = (8πan(0, z))−1/2 calculated at the position z.

Quantized vortices

255

For r⊥ ξz the solution should instead coincide with the unperturbed ground state wave function Ψv = n0 (r⊥ , z). (14.37) The functions (14.35)–(14.37) clearly match in the region ξz r⊥ R⊥ (z) so that the solution of the Gross-Pitaevskii equation is determined everywhere. Of course this procedure requires that R⊥ (z) ξz , a condition which is less and less satisﬁed as z → Z. The above solution can be used to calculate the energy of the vortex, yielding the result (Lundh et al., 1997) Ev =

4π 2 0.67R⊥ n0 Z ln , 3 m ξ

(14.38)

which holds beyond logarithmic accuracy and generalizes the result (5.32) derived for uniform gases in cylindrical geometry. Here n0 is the central density in the absence of vortices and ξ is the corresponding value of the healing length. It is worth noticing that the factor in front of the logarithm in eqn (14.38) can be straightforwardly derived from result (5.32) obtained in the cylindrical geometry, by replacing the quantity Ln with the z-integral of the condensate density along the symmetry axis (here L is the height of the cylinder). In fact, using the Thomas Fermi proﬁle (14.36), one ﬁnds ndz = (4/3)Zn0 . Of course this procedure, which can be extended to calculate the energy of a vortex displaced from the symmetry axis (see Section 14.8) provides the energy only within logarithmic accuracy. The Thomas–Fermi estimate (14.38) turns out to be in good agreement with the numerical calculations for large values of N . By 2 using the Thomas–Fermi relationship n0 = (15/8π)N/(ZR⊥ ) one obtains the result Ωcr =

5 0.67R⊥ 2 ln 2 mR⊥ ξ

(14.39)

for the critical angular velocity (Lundh et al., 1997). Typical values of Ωcr correspond to a fraction of the radial trapping frequency. Quantized vortices in trapped Bose gas have become experimentally available using diﬀerent approaches. A ﬁrst procedure consists of creating the vortical conﬁguration with optical methods in the two-component condensates discussed in Section 21.1 (Matthews et al., 1999). This technique is based on a coherent process involving the spatial and temporal control of interconversion between the two components. In this way one can create a vortex in one of the two components, the second one ﬁlling the core and hence providing a sort of pinning of the vortex. This technique is particularly useful for investigating the precession of the vortex (see Section 14.8). A second method, which shares a closer resemblance with the rotating bucket experiment of superﬂuid helium, makes use of a suitable rotating modulation of the trap to stir the condensate (Madison et al., 2000). Above a critical angular velocity one observes the formation of the vortex which is imaged after expansion. In fact, in situ measurements cannot provide any evidence of the vortex core, whose size (typically less than one micron) is too small. After expansion the size of the vortex is instead

256

Superﬂuidity and Rotation of a Trapped Bose Gas

Figure 14.9 Absorption images of a Bose–Einstein condensate containing up to thirteen ´ vortices in the Ecole Normale Sup´erieure (ENS) experiment. Source: Courtesy of Frederic Chevy (2001).

enlarged and becomes visible. A typical picture is shown in Figure 14.9, where one can see that, at suﬃciently high angular velocities, arrays with more vortices are also formed. The proﬁles measured after expansion can be compared with the theoretical predictions obtained solving the time-dependent Gross-Pitaevskii equation during the expansion. The comparison (see Figure 14.10) reveals a general agreement, although the experimental results indicate a partial ﬁlling of the core which is not predicted by theory. The discrepancy can be due to several eﬀects. In particular, it is likely that the vortex line exhibits a bent structure which results in a reduced visibility of the signal.

Quantized vortices

257

Column density [a.u.]

0.8 0.6 0.4 0.2 0 280

320

360

400

440 z [μm]

480

520

560

600

Figure 14.10 Density proﬁle of a single vortex after expansion. The experimental points are from Madison et al. (2000). The solid line is the theoretical calculation of Dalfovo and Modugno (2000).

The critical angular frequency observed in the experiments of Madison et al. (2000) turns out to be a factor of two larger than the theoretical prediction given by eqn (14.39) based on the condition of energetic stability. This indicates that for such values of Ω the nucleation of vortices is inhibited by the occurrence of a barrier. A possible mechanism of nucleation of vortices is actually suggested by the discussion of √ Section 14.5, where we have shown that, above the angular velocity Ω = ω⊥ / 2, the system spontaneously generates a deformation of quadrupole shape. This mechanism is expected to drastically suppress the barrier, thereby favouring the formation of vortices. In general, one predicts that if the rotating potential contains a deformation of multipolarity the instability of the system against the formation of surface deformations takes place for angular velocities larger than ω / (Dalfovo and Stringari, 2001). There is important experimental evidence in favour of this mechanism of nucleation of vortices. First, the observed critical angular velocity is rather close to the value √ ω⊥ / 2 associated with the quadrupole instability. Second, the nucleation process is associated with the occurrence of sizeable quadrupole deformations before the system reaches the equilibrium conﬁguration containing the vortex lines (see Figure 14.11). Finally, by adding an octupole deformation to the rotating potential the√nucleation is observed at smaller angular velocities, consistently with the value ω⊥ / 3 predicted by the condition of surface instability. The above mechanism can explain the nucleation of vortices if the stirring anisotropy is turned on rapidly at a ﬁxed value of Ω. If instead the angular velocity or the anisotropy of the trap are turned on adiabatically then diﬀerent scenarios take place (Madison et al., 2001). For example, if one makes an adiabatic ramping of Ω the system√will follow the normal branch discussed in Section 14.5 to well above the value ω⊥ / 2 until a dynamic instability occurs (see Figure 14.7). The threshold mechanisms discussed above imply a signiﬁcant hysteresis when the rotation frequency is ﬁrst speeded up to produce vortices and then slowed down again, since one expects

258

Superﬂuidity and Rotation of a Trapped Bose Gas

0.4 0.3

~

|α|

0.2 0.1 0.0

0

150

300

450

600

Time [ms]

Figure 14.11 Measurement of the time dependence of α ˜ (see Figure 14.7) when the stirring anisotropy is turned on rapidly. Five images taken at intervals of 150 ms show the transverse proﬁle of the elliptic state and reveal the nucleation of vortices. The size of each image is 300 μm. From Madison et al. (2001). Reprinted with permission from Physical Review Letters, c 2001, American Physical Society. 86, 4443;

diﬀerent mechanisms for the two processes: the nucleation of the vortex at relatively high rotation frequency and the destabilization of the vortex at lower frequency (see Section 14.8). At higher angular velocities more vortices can be formed, giving rise to a regular vortex lattice (see Figure 14.12). This lattice typically has a triangular shape, similar to what happens in superconductors (Abrikosov, 1957). In this regime the angular momentum acquired by the system approaches the classical rigid-body value and the rotation is similar to the one of a rigid body, characterized by the law ∇ × v = 2Ω. Using result (14.31) for the quantization rule and averaging the vorticity over several ˆ, where nv is the number of vortices per unit vortex lines one ﬁnds ∇ × v = (π/m)nv z area, related to the angular velocity Ω by the relation nv =

m Ω. π

(14.40)

Result (14.40) shows, in particular, that the distance between vortices (proportional √ to 1/ nv ) depends on the angular velocity but not on the density of the gas. Thus the vortices form a regular lattice even if the average density is not uniform as happens in the presence of harmonic trapping. This feature is conﬁrmed by experiments and can be used to check the quantization rule (14.31) by directly measuring the vortex density (14.40) as a function of the angular velocity Ω (Raman et al., 2001). Alternatively, the quantization of the circulation can be checked by measuring the angular

Vortices, angular momentum, and collective oscillations

259

Figure 14.12 Vortex lattices in the MIT experiment. From Ketterle (2001).

momentum (14.32) of a single vortex line through the precession of the quadrupole oscillation (see eqn (14.52)). At large angular velocities the vortex lattice is responsible for a bulge eﬀect associated with the increase of the radial size of the cloud and consequently with a modiﬁcation of the aspect ratio. In fact, in the presence of an average rigid rota2 tion, the eﬀective potential felt by the atoms is given by Vho − (m/2)Ω2 r⊥ . The new Thomas–Fermi radii then satisfy the relationship ω 2 − Ω2 Rz2 = ⊥ 2 , 2 R⊥ ωz

(14.41)

showing that at equilibrium the angular velocity can not overcome the radial trapping frequency. This formula can be used to directly determine the value of Ω by just measuring the in situ aspect ratio of the atomic cloud. This is particularly useful when, after stirring the condensate, one no longer has an external control of its angular velocity Ω. When the angular velocity Ω becomes too close to the centrifugal limit ω⊥ the three-dimensional Thomas–Fermi picture is no longer valid and eventually the system becomes two-dimensional. New, important phenomena take place in two dimensions, especially when one approaches the lowest Landau level (LLL) and the quantum Hall regimes. Some of these features will be discussed in Section 23.3. Let us ﬁnally recall that vortices with double vorticity can be created using topological imprinting techniques (Shin et al., 2004). They have, however, been shown to exhibit dynamic instability.

14.7

Vortices, angular momentum, and collective oscillations

In this section we discuss the eﬀects of the vortex on the macroscopic oscillations of the system, i.e. on those oscillations which can easily be driven by a suitable modulation

260

Superﬂuidity and Rotation of a Trapped Bose Gas

of the conﬁning trap. In the absence of vortices these oscillations were discussed in Sections 12.1 and 12.2. A key peculiarity of the vortex is that it breaks time-reversal invariance. Therefore, one expects that states with opposite values of the third component m of angular momentum, which were degenerate in the absence of the vortex, will now have diﬀerent frequencies. A simple way to calculate the corresponding splitting ωm −ω−m is provided by the sum rule approach. This method avoids the complications of a complete solution of the Gross-Pitaevskii equation. Furthermore, it emphasizes explicitly the role of the relevant symmetries of the problem. Let us consider the most important case of the quadrupole oscillations excited by the operators ˆ± = Q (xk ± iyk )2 , (14.42) k

ˆ† = Q ˆ −. carrying m = ±2 units of angular momentum and satisfying the relationship Q + We know that in the absence of vortices the operators (14.42) excite, in the Thomas– √ Fermi limit, two collective quadrupole modes with frequency ω± = 2ω⊥ . Our aim is to discuss how this result is modiﬁed by the presence of the vortex which is expected to remove the degeneracy between the two modes. According to the general deﬁnitions introduced in Chapter 7, we can deﬁne the dynamic structure factor relative to the above quadrupole operators: ˆ ± |m |2 δ(ω − ωnm ), S± (ω) = Q−1 e−βEm | n|Q (14.43) m,n

where Q = m exp(−βEm ) is the partition function and ωnm = (En − Em ). By introducing the moments +∞ p+1 ˆ ± |m |2 (ωnm )p m± = dωS± (ω)ω p = Q−1 e−βEm | n|Q (14.44) p −∞

m,n

and using the completeness relation (see Section 7.1) one easily obtains the following exact results for the m = ±2 sum rules: − m+ 0 − m0 = [Q− , Q+ ] = 0, − m+ 1 + m1 = [Q− , [H, Q+ ]] = 8N

(14.45)

2 2 r , m ⊥

(14.46)

and − m+ 2 − m2 = [[Q− , H], [H, Q+ ]] = 16N

3 z , m2

(14.47)

where z = Lz /N is the average value of the angular momentum per particle. It is worth pointing out that the breaking of time-reversal symmetry shows up explicitly in − the diﬀerence m+ 2 − m2 , which turns out to be proportional to the angular momentum

Vortices, angular momentum, and collective oscillations

261

of the system. The sum rule approach becomes particularly useful if one assumes that the moments m± p are exhausted by two modes with frequency ω± . Then the dynamic structure factor can be written in the form S± (ω) =

1 [σ± δ(ω − ω± ) − σ∓ δ(ω + ω∓ )], 1 − exp(−βω)

(14.48)

which satisﬁes the detailed balancing principle (7.6). Equation (14.45) implies σ+ = σ− ≡ σ, while the other two sum rules can be expressed in terms of ω± and σ as − + − 2 2 m+ 1 + m1 = σ(ω+ + ω− ) and m2 − m2 = σ(ω+ − ω− ). One then obtains the nontrivial result ω+ − ω− = 2

z 2 mr⊥

(14.49)

for the frequency splitting of the two quadrupole modes (Zambelli and Stringari, 1998). In the presence of a single quantized vortex located along the symmetry axis the angular momentum is given by z = , so that the measurement of the frequency splitting can be regarded as a way to check the quantization of angular momentum. It is worth pointing out that, using the same sum rule approach, no splitting is predicted for the dipole excitation induced by the operators D± = x ± iy. In fact, in this case the operators [H, D± ] = −i(px ± ipy )/m commute each other with the − consequence that m+ 2 = m2 and hence also ω+ = ω− in the presence of the vortex. This result is consistent with the fact that the dynamics of the motion of the centre of mass are completely ﬁxed by the external potential and are not sensitive to the internal structure of the many-body wave function. A diﬀerent result is obtained in the rotating frame, where the Hamiltonian contains the additional term −ΩLz . In this case the commutator [H, D± ] contains an additional term: [H, D± ] = −i(px ± ipy )/m ∓ ΩD± and the sum rule (14.47) no longer vanishes. The ﬁnal result for the splitting of the dipole frequencies in the rotating frame is ω+ − ω− = −2Ω. For large angular velocities, when a vortex lattice is formed and one can safely replace the discretized vorticity (5.27) with the average value ∇ × v = 2Ω corresponding to a rigid ﬂow, one can calculate the collective frequencies using the equations of rotational hydrodynamics. These equations diﬀer from those holding for an irrotational ﬂuid (see eqn (12.6) due to an additional term in the equation for the velocity ﬁeld, depending explicitly on the curl of v: ∂v 1 m +∇ mv 2 + Vext + gn = mv × (∇ × v). (14.50) ∂t 2 In the presence of harmonic trapping the solution of the linearized hydrodynamic equations yields the simple dispersion law (Cozzini and Stringari, 2003a) # 2 ω± = 2ω⊥ − Ω2 ± Ω (14.51) for the quadrupole frequencies. The splitting of 2Ω between the two frequencies is consistent with the sum rule result (14.49) once one employs the rigid value expres2 sion z = mΩ r⊥ for the angular momentum. Prediction (14.51) for the m = ±2

262

Superﬂuidity and Rotation of a Trapped Bose Gas (a) 18

(b) 0.8 (ω+–ω–)/(2ω )

ω/2π [Hz]

14

10

6

0.4

2 0.6

0.6

0.8

1.0

1.2

1.4

1.6

0.4

λBEC

0.6 Ωeff/ω

0.8

Figure 14.13 Quadrupole surface wave spectroscopy of condensates formed in a rotating normal cloud. (a) The quadrupole frequency as a function of the condensate aspect ratio λBEC = Rz /R⊥ for the m = +2 (squares) and m = −2 (triangles) surface waves. In (b) the results for the frequency splitting are shown as a function of the angular velocity of the condensate inferred from the measured aspect ratio via eqn (14.41). The solid line corresponds to the theoretical prediction (14.51). From Haljan et al. (2001b). Reprinted with permission c 2001, American Physical Society. from Physical Review Letters, 86, 210403;

quadrupole frequencies has been conﬁrmed experimentally with remarkable accuracy in the experiment by Haljan et al. (2001b), where the two m = ±2 quadrupole frequencies have been separately measured for diﬀerent rotating conﬁgurations. In this experiment the ratio ω⊥ /ωz was equal to 1.53 and values of Rz /R⊥ down to 0.54 were observed corresponding to Ω = 0.94ω⊥ . Figure 14.13 shows the good agreement between theory and experiment both for the splitting (b) and for the two separate quadrupole frequencies (a). A more direct measurement of the splitting (14.49), and hence of the angular momentum carried by the system, is provided by studying the precession of the quadrupole deformation of a condensate containing one or more vortex lines. Let us suppose that a quadrupole perturbation of the form Vpert = K k (x2k − yk2 ) is suddenly applied to the system for a short time interval. The perturbation generates quadrupole oscillations which exhibit precession in the x–y plane if ω+ = ω− . The precession is easily calculated, taking into account that in the frame rotating with the angular velocity dφ/dt, where the angle φ ﬁxes the symmetry axis of the deformed conﬁguration, the two quadrupole frequencies should be equal, i.e. ω+ − 2dφ/dt = ω− + 2dφ/dt. This yields the result dφ ω+ − ω− z = = 2 . dt 4 2m r⊥

(14.52)

In Figure 14.14 we show a series of nondestructive images of the quadrupole mode excited using this procedure (Haljan et al., 2001a). The ﬁgure explicitly shows the

Vortices, angular momentum, and collective oscillations (a)

(b)

(c)

263

(d) 50

25

45.5 ms

∆θ [º]

0 ms

0 (a)

–25

(b) (c)

91 ms

–50 0

100 Time [ms]

200

136.5 ms

182 ms

227.5 ms

Figure 14.14 The use of surface excitations for in situ detection of a vortex in a conﬁned BEC. (a), (b), and (c) are each a series of nondistructive images of the quadrupole mode after excitation. (a) is the case of a vortex-free condensate; the observed precession of the principal axis in (b) and (c) reveals the presence of a vortex. Vortices in (b) and (c) have opposite angular momentum. The precession frequency is measured with a linear ﬁt, as shown in (d). From Haljan et al. (2001a). Reprinted with permission from Physical Review Letters, c 2001, American Physical Society. 86, 2922;

precession due to the presence of the vortex. The above technique provides an eﬃcient tool with which to measure the frequency splitting and hence the angular momentum carried by the vortical conﬁgurations. In particular it has been used to explicitly prove the quantization of angular momentum (see Figure 14.15) (Chevy et al., 2000). This experiment shares interesting resemblances with the Vinen experiment discussed in Section 8.4, where, by measuring the lift of degeneracy between the vibrational modes of a thin wire placed at the centre of the rotating ﬂuid, it was possible to prove the quantization of the circulation in superﬂuid 4 He (see Figure 8.11). The same method has been used to measure the moment of inertia of a superﬂuid Fermi gas, revealing the quenching eﬀect caused by irrotationality (see Section 19.7). It is also interesting to mention that the splitting of the dipole oscillation exhibited in the rotating frame (see discussion in the second paragraph following eqn (14.49)) would

264

Superﬂuidity and Rotation of a Trapped Bose Gas

3.0

Lz/ħ

2.0 1.0 0.0 110

115

120 125 130 135 Stirring frequency [Hz]

140

145

Figure 14.15 Variation of angular momentum per particle deduced from eqn (14.52) as a function of the stirring frequency Ω for ω⊥ /2π = 175 Hz. From Chevy et al. (2000). Reprinted c 2000, American Physical Society. with permission from Physical Review Letters, 85, 2223;

give rise to a precession rate equal to dφ/dt = Ω, in analogy with the famous precession of the Foucault pendulum, Ω being related to the Earth angular speed by the relation Ω = ΩEarth sin φ, where φ is the latitude. In addition to the shape oscillations of hydrodynamic nature discussed above, a vortex lattice exhibits another class of excitations originating from its elastic nature. The theory of these oscillations was developed by Tkachenko (1966) for an incompress ible superﬂuid, predicting the dispersion law ωT = Ω/4m, where Ω is the angular velocity of the rotating ﬂuid, related to the number of vortices per unit surface by the relation (14.40). The frequency ωT is calculated in the rotating reference frame, where the vortex lattice is at rest and the Hamiltonian is given by H = H0 − ΩLz . The theory of the Tkachenko modes was later further developed by Baym and Chandler (1983, 1986) who generalized the hydrodynamic theory of superﬂuids taking into account the elasticity of the vortex lattice. The eﬀects of the compressibility on the Tkachenko modes were discussed in detail by Sonin (1987) who derived the relevant dispersion law ωT2 =

Ω c2 q 4 2 4m 4Ω + c2 q 2

(14.53)

for the elastic oscillations holding in the Thomas–Fermi regime mc2 Ω, where the healing length /2mc, providing the width of the vortex, is much smaller than the distance /mΩ between vortices. Result (14.53) reproduces the original Tkachenko result for large values wave vectors (q Ω/c), while it gives rise to the quadratic dispersion /16mΩcq 2 in the opposite limit, revealing the crucial role played by the compressibility of the system. The transition between the quadratic and the linear q dependence takes place at values q ∼ Ω/c which, in trapped condensates, can be signiﬁcantly larger than the inverse of the radial size of the system. This suggests that the eﬀects of compressibility play a crucial role in the Tkachenko modes of a trapped gas. In addition to the Tkachenko oscillation, a gapped branch is predicted to occur

Vortices, angular momentum, and collective oscillations

265

with dispersion ω 2 = 4Ω2 + c2 q 2 (Baym, 2003) approaching the usual phonon branch when Ω → 0. Due to the gapped nature of the phonon branch one can easily prove that in the limit of small q the compressibility sum rule (7.52) is exhausted by the Tkachenko mode. The gapped branch instead exhausts the f-sum rule (7.48) in the same q → 0 limit (Cozzini et al., 2004). The existence of the gap in the phonon branch is a direct consequence of the fact that in the rotating frame the current operator, deﬁned by the commutator (7.45) between the Hamiltonian and the density operator ρ, is not a conserved quantity in the q → 0 limit, due to the presence of the −ΩLz term in the Hamiltonian. The behaviour of the Tkachenko oscillations in the presence of harmonic trapping was investigated by Anglin and Crescimanno (2002) and Baym (2003), who calculated the discretized frequencies taking into account the ﬁnite and inhomogeneous nature of the system. Fully numerical calculations of the Tkachencko waves in harmonically trapped gases have also been carried out using Gross-Pitaevskii theory (Simula et al., 2002; Baksmaty et al., 2004; Mizushima et al., 2004; Woo et al., 2004) and the sum rule approach (Cozzini et al., 2004). The ﬁrst experimental excitation of the Tkachenko modes in trapped gases was obtained by Coddington et al. (2003) through selective removal of atoms from the centre of the condensate (see Figure 14.16). In Figure 14.17 we show the comparison between the experimental frequencies and the

Figure 14.16 Tkachenko mode excited by atom removal. BEC rotation is counterclockwise. Lines are sine ﬁts to the vortex lattice. From Coddington et al. (2003). Reprinted with c 2003, American Physical Society. permission from Physical Review Letters, 91, 100402;

266

Superﬂuidity and Rotation of a Trapped Bose Gas 5

4

ωT/ω0

3

2

1

0 0.85

0.9

0.95

1

Ω /ω 2 Figure 14.17 Lowest Tkachenko frequency of a trapped Bose gas in units of ω0 = Ω/4mR⊥ as a function of the angular velocity Ω. The solid line is the sum rule result, while the dashed line is the prediction of eqn (14.53) with q = 5.45/R⊥ (see text). Experimental points are taken from Coddington et al. (2003) and Schweikhard et al. (2004) using the three-dimensional Thomas–Fermi value for R⊥ . From Cozzini et al. (2004).

theoretical predictions by Cozzini et al. (2004). The dashed line in the ﬁgure is the prediction of eqn (14.53) using the estimate q = 5.45/RT F calculated by Anglin and Crescimanno (2002). For a review on the Tkachenko oscillations, see, for example, Sonin (2013).

14.8

Stability and precession of the vortex line

In the previous section we investigated precession phenomena which involve the motion of the condensate in the presence of vortices. Another important class of phenomena is given by the precession of the vortex line with respect to the condensate. This motion is directly related to the conditions of stability of the vortical conﬁguration. In Section 14.6 we discussed the conditions of stability for a vortex line. Stability is ensured if the trap rotates fast enough. For low angular velocities the vortex is unstable against the creation of elementary excitations and its motion will be destabilized in a continuous way in the presence of dissipative phenomena. In the simplest case one expects the destabilization to take the form of a spiral motion of the vortex line towards the periphery. For a ﬁrst description of these processes it is useful to make some simplifying assumptions. A crucial step is to assume that the vortex line remains parallel to the symmetry axis of the trap. This is expected to be a reasonable assumption in the case of a pancake-like geometry where bending eﬀects in the vortex line are not expected to be very important. Conversely, in the case of cigar-shaped conﬁgurations the eﬀects of bending can be important (Garc´ıa-Ripoll and P´erez-Garc´ıa, 2001).

Stability and precession of the vortex line

267

Let us calculate the angular momentum and the energy of a straight vortex line displaced by a distance d from the axis of the trap. By assuming that the healing length is small and that the density proﬁle is not aﬀected by the vortex on a macroscopic scale, the angular momentum is easily calculated. One rewrites the angular momentum (14.32) in cylindrical coordinates (r⊥ , ϕ, z) with the z-axis chosen along the axis of the trap: Lz = m dz r⊥ dr⊥ dϕr⊥ vϕ n(r⊥ , z) = m dz r⊥ dr⊥ n(r⊥ , z) v · dl. (14.54) The contour of integration is a circle of radius r⊥ around of the axis of the trap. The integrand of (14.54) vanishes for r⊥ ≤ d, where d is the distance of " the vortex line from the symmetry axis of the trap. Conversely, for r⊥ ≥ d one has v · dl = 2π/m. Using the Thomas–Fermi proﬁle for the density distribution we ﬁnally obtain 5/2 d2 Lz = N 1 − 2 , R⊥

(14.55)

showing that the angular momentum reduces as d increases. Notice that the resulting dependence of Lz on the distance d diﬀers from the one derived in Section 6.8 in cylindrical geometry, as a consequence of the harmonic shape of the trapping potential. The energy can also be calculated in easy way, if one works within logarithmic accuracy. To this purpose it is suﬃcient to replace the quantity Ln entering eqn (5.32) with the integral ndz evaluated with the unperturbed density (14.36) calculated 2 3/2 at r⊥ = d. A simple integration yields the result ndz = n0 Z(4/3) 1 − d2 /R⊥ , showing that the displacement of the vortex results in the simple dependence 3/2 d2 Ev (d) = Ev (0) 1 − 2 , R⊥

(14.56)

where Ev (0), is the energy (14.38) of the vortex placed on the symmetry axis of the trap. From equation (14.56) it follows that the position of the vortex on the axis of a non-rotating trap corresponds a maximum of energy and hence to an unstable conﬁguration (Dodd et al., 1997; Rokhsar, 1997). If the trap rotates with angular velocity Ω , the energy in the rotating frame can be obtained combining (14.55) and (14.56) and takes the form (Fetter and Svidzinsky, 2001): 3/2 5/2 Ev (d, Ω) d2 d2 = Ωcr 1 − 2 − Ω 1 − 2 , N R⊥ R⊥

(14.57)

where Ωcr is the critical angular velocity (14.39). This expression has a maximum at d = 0 if Ω < 35 Ωcr ; conversely, it has a minimum if Ω > 35 Ωcr . In the interval 3 5 Ωcr < Ω < Ωcr the vortex is metastable, while for Ω > Ωcr the vortex corresponds to the ground state of the system and is consequently stable unless the creation of two or more vortices becomes energetically more preferable. The above discussion

268

Superﬂuidity and Rotation of a Trapped Bose Gas 0.6 Ω/Ωcr = 0.4

Ev/Ev(0)

0.4 Ω/Ωcr = 0.9

0.2 0

Ω/Ωcr = 1.3

−0.2 −0.4

0

0.2

0.4

0.6

0.8

1

d/R

Figure 14.18 Energy of a vortex as a function of its distance d from the symmetry axis for diﬀerent values of the angular velocity of the trap.

thus shows in an explicit way that the vortex is stabilized by the rotation of the trap (see Figure 14.18). If the vortex is placed at distance d from the symmetry axis it will exhibit precession and, in the absence of dissipation, it will follow a circular orbit around the axis. The angular velocity of the precession in the rotating frame can be easily calculated using the general equation Ωprec = ∂Ev /∂Lz . Using result (14.57) one gets Ωprec =

3 ∂Ev /∂d Ωcr = 2 − Ω, ∂Lz /∂d 5 1 − d2 /R⊥

(14.58)

showing that not only the modulus, but also the sign of Ωprec depends on the actual value of Ω. This has important consequences at ﬁnite temperatures where, as a consequence of dissipative processes, the vortex will move in the direction of minimum energy. If Ωprec > 0 (corresponding to ∂Ev /∂d < 0) the vortex will move towards the periphery of the condensate where it will eventually disappear. In the opposite case (Ωprec < 0) the vortex will instead move towards the centre of the trap. It is worth recalling that result (14.58) is based on the assumption of a straight vortex line, which is a safe approximation for disk-shaped condensates. For a systematic discussion of the stability of vortices see Fetter and Svidzinsky, 2001. When the displacement is small the precession of the vortex can be regarded as a small oscillation of the system around the stationary d = 0 vortical conﬁguration. This oscillation takes the form of a circularly polarized dipole motion and is also called the anomalous dipole mode. Its precession frequency is given by Ωprec =

3 Ωcr − Ω . 5

(14.59)

Quantized vortices and critical velocity in a toroidal trap

269

(a)

50 ms

0 ms

150 ms

100 ms

200 ms

250 ms

300 ms

(b)

(c) 45

(d) 15

0 –45

r/ ξ

θt [º]

10

5

–90 –135

0

100 200 Time [ms]

300

0

0

100 200 Time [ms]

300

Figure 14.19 (a) Vortex core precession observed with nondestructive images using twocomponent condensates. (b) Corresponding ﬁt to the density proﬁles. (c) A linear ﬁt to the data indicates a precession frequency of 1.3 Hz. (d) Core radius in units of the healing length. This vortex core should not be confused with the vortex core exhibited by a single-component condensate. From Anderson et al. (2000). Reprinted with permission from Physical Review c 2000, American Physical Society. Letters, 85, 2857;

For Ω < 35 Ωcr the energy change (14.57) associated with this mode is negative. According to the general discussions of Section 5.6, this solution is consequently characterized by a negative excitation energy ωi = −Ωprec , reﬂecting its energetic instability. Furthermore, following the same procedure developed in Section 6.8, one ﬁnds that the angular momentum of this mode is equal to −. Notice that the relationship ωi = −Ωprec also holds for the Kelvin modes discussed in Section 6.8. However, in that case the modes have positive energy and the precession frequency is negative, i.e. opposite to the velocity ﬁeld generated by the vortex line. Direct experimental evidence for the precession of the vortical line has been shown in the experiment of Anderson et al. (2000) (see Figure 14.19) and, more recently, by Freilich et al. (2010). Investigations into the dissipative eﬀects responsible for the spiral motion of the vortex line at ﬁnite temperatures have been made by Fedichev and Shlyapnikov (1999).

14.9

Quantized vortices and critical velocity in a toroidal trap

In Section 14.8 we discussed the stability of vortex lines and shown that, if the harmonic trap does not rotate, the vortex does not correspond to a conﬁguration of minimum energy and its motion will be destabilized in the presence of dissipative phenomena.

270

Superﬂuidity and Rotation of a Trapped Bose Gas

The situation is diﬀerent if we stabilize the vortex with a pinning potential (Simula et al., 2002). The realization of toroidal traps provides a particularly eﬃcient way to stabilize the rotating ﬂow and to generate permanent currents. Toroidal conﬁgurations can be realized using blue-detuned lasers which make a repulsive potential barrier in the middle of a harmonic magnetic trap so that, in the case of cylindrical symmetry, the external potential felt by atoms takes the form Vext =

2 2 1 2 2 m ω⊥ ρ + ωz2 z 2 + V0 e−2ρ /w0 , 2

(14.60)

where ρ2 = x2 + y 2 and we have assumed a Gaussian proﬁle for the repulsive laser potential, with V0 proportional to the laser intensity. The laser beam repels atoms from the trap centre, creating a BEC density distribution with a hole in the centre if V0 is larger than the chemical potential. Hence, this trap geometry can be conveniently changed from simply to multiply connected by increasing the laser power. Similarly, changing the intensity and size of V0 changes the radii and shape of the toroidal trap. Traps of this type have been employed to generate persistent currents with quantized circulation which survive for several seconds (Ryu et al., 2007). The eﬀect of the circulation in a toroidal trap can be revealed looking at the density proﬁle after expansion. In fact, in the absence of the current the expansion ﬁlls the initial hole generated by the potential (14.60) while, in the presence of the current, the hole will survive after the expansion due to the repulsive role caused by the centrifugal eﬀect (Cozzini et al., 2006). This eﬀect was explicitly observed by Ryu et al. (2007). The toroidal geometry is particularly suitable to investigate the critical velocity of the superﬂuid ﬂow through a repulsive barrier (see Section 14.1) and the occurrence of phase slip phenomena. The problem was investigated theoretically by Piazza et al. (2009) by solving numerically the time-dependent Gross Pitaevskii eqn (5.2). Initially the trap was cylindrically symmetric and a persistent current with quantized circulation was excited. Then a standing repulsive barrier was adiabatically raised. It occurs that this violation of cylindrical symmetry in the presence of the current results in the creation of numerous vortices and antivortices in the region of very low density outside the condensate. The process of the phase slip can be directly visualized and is quite nontrivial. There are two diﬀerent critical barrier heights. At the smaller critical height a single-quantized vortex line moves from the internal region outside the torus and enters the annulus in the vicinity of the barrier, leaving behind a 2π phase slip. When the vortex reaches the dense part of the condensate, it begins to circulate with the ﬂow without crossing it completely. This means that the vortex decreases the angular momentum of the condensate only by a fraction of . If the barrier reaches the higher critical height, a single-quantized antivortex enters the annulus from the outward low-density region. Diﬀerent scenarios exist, depending on the width of the annulus, the barrier height, and the ramping time. Vortices and antivortices can circulate on separate orbits, or can collide and annihilate. When they annihilate (or circulate on nearby orbits) the system undergoes a 2π phase slip and the angular momentum decreases by . Direct measurements of the critical velocity for a condensate in a toroidal trap were performed by Wright et al. (2014). A condensate of 7.6 × 105 of atoms of 23 Na was

Quantized vortices and critical velocity in a toroidal trap

271

Critical barrier height Uc /h [kHz]

2.0 1.8 1.6 1.4 1.2 1.0 0.8 0.6 0.4 0.2 0.0

0

5

25 20 15 10 Barrier angular velocity Ω/2π [Hz]

30

35

Figure 14.20 Measured critical barrier height Uc as a function of angular velocity of the rotating potential barrier. The dashed line corresponds to the theoretical prediction of eqn (14.61). From Wright et al. (2014). Reprinted with permission from Physical Review c 2013, American Physical Society. A, 88, 063633;

trapped in a toroidal potential Vtrap = m[ωz2 z 2 + ωρ2 (ρ − R)2 ]/2 derivable from (14.60) in the harmonic approximation. The large radius of the torus was R = 22.6μ, while the Thomas–Fermi width of the condensate in the radial direction was 22 μm and the vertical thickness was about 5 μm. The repulsive potential barrier was created by a blue-detuned vertical beam focused to a circular spot of diameter 9μm. The healing length ξ ≈ 0.3 μm was small enough to use the LDA approximation. The barrier ‘stirs’ the condensate, performing rotational motion along the torus with angular frequency Ω. After the stirring procedure, the authors investigated the appearance of the circulation in the condensate, by observing the persistence of a hole in the density proﬁle after release of the trap. In this way it was possible to measure the critical velocity as a function of the barrier height Vmax . In order to compare their results with theory, Wright et al. (2014) reduced the three-dimensional problem to one dimension, performing proper integrations along the z and ρ directions. As a result, they obtained an equation, analogous to eqn (14.2): 2 2/5 mvcr 5 m vcr c4∞ = 2mc2∞ − Vmax , − 4 4

(14.61)

where c∞ = gn∞ /2m and n∞ is the density far from the constriction. In Figure 14.20 the critical height of the barrier, at which the circulation is created, is shown as a function of the angular velocity Ω of the barrier and compared with the theoretical prediction (14.61). Theoretical and experimental results agree in a reasonable way.

15 Coherence, Interference, and the Josephson Eﬀect An important consequence of Bose–Einstein condensation is the occurrence of coherence eﬀects associated with the phase of the order parameter. In the previous chapters (see in particular Chapter 5) we have often pointed out that the order parameter behaves like a classical ﬁeld, obeying the nonlinear Gross-Pitaevskii diﬀerential equation. This suggests the existence of interesting analogies with the coherence phenomena exhibited by light. On the other hand, the important role played by interactions suggests the occurrence of analogies with the coherence phenomena typical of superﬂuids and superconductors. The problem of the coherence of a single trapped Bose gas is addressed in Section 15.1, where we discuss the robustness of Bose–Einstein condensation against fragmentation and we point out the eﬀects of long-range order on the one-body density matrix. In the following sections we discuss the eﬀects of coherence relative to two or more condensates. Also, in this case several physical phenomena can be accurately described within the mean-ﬁeld scheme, where the order parameter behaves classically. In Section 15.2 we discuss the interference patterns produced by two overlapping condensates, while in Section 15.3 we consider the Josephson oscillations in the double-well potential. The mean-ﬁeld picture, based on the use of the Gross-Pitaevskii equation, is in general expected to provide an accurate description of the behaviour of a Bose–Einstein condensate in the large N limit. However, if the system is made of two or more separated condensates, quantum eﬀects may become important even if N is large. In particular, under special conditions, the behaviour of the phase can reveal new features which cannot be described within the classical mean-ﬁeld scheme. In Section 15.4 we address the problem of the quantum description of the Josephson oscillation and of the ﬂuctuations of the phase which can introduce deep changes in the behaviour of the system, giving rise, for example, to number-squeezed conﬁgurations. In Section 15.5 we brieﬂy investigate the decoherence mechanisms of the phase, while in Section 15.6 we discuss the Josephson eﬀect in the limit of the quasi-ideal gas, employing the formalism of the boson Hubbard Hamiltonian. The boson Hubbard Hamiltonian will also be used in Chapter 22 to discuss the behaviour of Bose gases in the context of periodical conﬁgurations.

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Coherence and the one-body density matrix

15.1

273

Coherence and the one-body density matrix

In the previous chapters we have implicitly assumed that Bose–Einstein condensates are ‘coherent’ objects, well described by the order parameter predicted by GrossPitaevskii theory. This assumption is not however completely obvious, even at zero temperature, because the system may prefer to occupy diﬀerent conﬁgurations which do not necessarily correspond to the macroscopic occupation of a single-particle state. The robustness of Bose–Einstein condensation against fragmentation is ensured by two-body interactions. The simplest way to see this important feature is to consider a uniform gas conﬁned in a box of volume V and to compare the energy of the two following conﬁgurations: the ﬁrst (full Bose–Einstein condensation) corresponds to √ putting all the atoms in the p = 0 single-particle state φ0 = 1 V : 1 † N a0 |vac. |1 = √ N!

(15.1)

The second conﬁguration (fragmented Bose–Einstein condensation) is instead obtained by assuming that N0 atoms occupy √ the single-particle state φ0 and N1 atoms the ﬁrst excited state φ1 = exp(ip1 · r/)/ V : |2 = √

† N0 † N1 1 a a1 |vac, N0 !N1 ! 0

(15.2)

with N1 + N2 = N . If one ignores the kinetic energy term, which is negligibly small in the macroscopic limit since p ∝ 1/V 1/3 , the energy of the many-body states |1 and by the average value of the interaction Hamiltonian Hint = |2 † is given ˆ (r)Ψ ˆ † (r)Ψ(r) ˆ Ψ(r). ˆ ˆ (g/2) drΨ Using the representation Ψ(r) = φ0 (r)ˆ a0 + φ1 (r)ˆ a1 for the ﬁeld operator it is then useful to calculate the energy diﬀerence ΔE = E2 − E1 between the two conﬁgurations. One ﬁnds: (15.3) ΔE = gN0 N1 dr|φ0 |2 |φ1 |2 . The energy diﬀerence (15.3) is macroscopically large because the two wave functions φ0 and φ1 fully overlap in space, showing that interactions play against BEC fragmentation if the coupling constant g is positive. The opposite happens if g is negative. This behaviour is the consequence of exchange eﬀects which are active in the fragmented conﬁguration (Nozi`eres, 1995). As discussed in Chapter 2, an important consequence of Bose–Einstein condensation is the occurrence of long-range order. Actually, full BEC implies that the one-body density of the ground state can be written as n(1) (r, r ) = Ψ∗ (r)Ψ(r ) = n(r) n(r ) . (15.4) The distance s = |r − r | at which the one-body density becomes negligible is called the coherence length. Equation (15.4) shows that the coherence length of a Bose– Einstein condensate is of the order of the size of the sample. Checking this behaviour experimentally is a question of high relevance, which touches the conceptual basis of Bose–Einstein condensation. Notice that experiments based on the imaging of single

274

Coherence, Interference, and the Josephson Eﬀect

condensates measure the diagonal density n(r) and consequently do not provide any information on long-range eﬀects. Information on the behaviour of the oﬀ-diagonal one-body density matrix is available from interferometry experiments as well as from the measurement of the momentum distribution. An important experiment in this direction is the analogue of the double-slit experiment (Bloch et al., 2000). The double slit for the trapped atoms is created using a radio wave ﬁeld with two frequency components acting on a single condensate trapped by a magnetic ﬁeld. This generates two slits located at diﬀerent heights from which atoms escape and propagate downwards as a result of gravity. The correlation function is then revealed by measuring the interference patterns generated by two propagating matter waves. The initial phase of each wave is ﬁxed by the value of the ﬁeld operˆ at the position z = ±d/2 of each slit so that the visibility of the interference ator Ψ ˆ † (z + d/2)Ψ(z ˆ − d/2), i.e. to the patterns will be proportional to the average value Ψ (1) one-body density matrix n (z + d/2, z − d/2). One can deﬁne the visibility factor according to V =

n(1) (z + d/2, z − d/2) , n(z)

(15.5)

where, in order to ensure that the diagonal density is uniform in the region between the two slits, we have assumed that the distance d is much smaller than the size of the condensate in the zth direction. The double-slit experiment is well suited to exploring the long-range behaviour of the system as a function of the distance d, which can be varied by changing the frequency components of the radio wave ﬁeld, as well as of the temperature. Figure 15.1 shows that for temperatures larger than the critical temperature for BEC (white circles and squares) the visibility tends to zero within distances which turn out to be slightly higher than the thermal wavelength λT = 2π2 /mk B T . This distance is much smaller than the axial size of the sample, since λT /Rz ωz /kB T . When the temperature is smaller than Tc the correlation function exhibits an important change of behaviour approaching a constant value. It eventually tends to zero at distances of the order of the size of the condensate. These results clearly point out the eﬀects of long-range order associated with the Bose–Einstein condensed component below Tc . The oﬀ-diagonal behaviour of the one-body density of the condensate can also be explored by measuring the dynamic structure factor S(q, ω) in the impulse regime (7.34) through two-photon Bragg scattering experiments. In fact, starting from eqn (7.34) and using the relationship (2.5) between n(p) and n(1) (r1 , r2 ), one can derive the useful relationship

s msz s = dωS(q, ω) exp −i (ω − ωr ) n(1) (s) = drn(1) r − , r + (15.6) 2 2 q for the oﬀ-diagonal one-body density, where s and q are vectors oriented along the z-direction and ωr = q 2 /2m is the free recoil frequency. Result (15.6) is exact if one works at suﬃciently large momentum transfers q where the dynamic structure factor is correctly approximated by the impulse approximation. In this limit the measured

Coherence and the one-body density matrix

275

1

Visibility

0.8 0.6 T = 250 nK T = 310 nK T = 450 nK T = 290 nK

0.4 0.2 0 0

100

200

300 400 Δz [nm]

500

600

700

Figure 15.1 Spatial coherence of a trapped Bose gas as a function of slit separation for temperature above (black crosses and circles) and below (white circles and squares) the transition temperature. For temperatures above Tc coherence disappears for distances much smaller than the size of the sample. (The number of atoms in the trap was reduced to prepare a thermal gas at a temperature of 290 nK.) From Bloch et al. (2000). Reprinted by permission c 2000, Macmillan Publishers Ltd. from Nature, 403, 168;

signal S(q, ω) can consequently be used to infer about the existence of long-range order in the sample. A peculiarity of the dynamic structure factor in dilute Bose gases is that the contributions of the condensate and of the thermal component are well separated, reﬂecting the diﬀerent behaviour of the two components in momentum space, as already discussed in Section 10.3. In particular, the width of the condensate and of the thermal contributions to the dynamic structure factor scale, respectively, like q/Rz and q/λT . According to (15.6), the narrower the signal S(q, ω) around the free recoil frequency ω, the weaker the decay of n(1) (s) at large distances. For example, if one chooses the Gaussian parameterization S(q, ω) ∝ exp[−(ω − ωr )2 /2Δ2 ], one obtains the result s2 n(1) (0, 0, sz ) = N exp − z2 , (15.7) 2χ the quantity χ = q/Δm playing the role of a coherence length. The above parameterization for√the one-body density matrix is exact in the classical regime T Tc , where χ = λT / 2π as well as for √ an ideal Bose gas trapped by a harmonic potential at zero temperature, where χ = 2az . It also provides an excellent approximation for a trapped Bose–Einstein condensate in the Thomas–Fermi regime, where one ﬁnds χ = Rz 3/8 (see eqn (12.75)). The fact that the coherence length is of the order of the size of the condensate reveals that in these systems the Heisenberg inequality Rz ΔPz ≥ /2 is close to an identity. The dynamic structure factor has been measured

276

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at high momentum transfer by Stenger et al. (1999), conﬁrming that the width of S(q, ω) in these trapped Bose–Einstein condensates is Heisenberg-uncertainty limited by their ﬁnite size. The Heisenberg-limited momentum spread was also recently conﬁrmed experimentally in a uniform interacting BEC (Gotlibovych et al., 2014).

15.2

Interference between two condensates

The simplest example of interference is provided by two initially separated condensates which, after releasing the conﬁning traps, expand and eventually overlap. This experiment was ﬁrst performed at MIT (Andrews et al., 1997b), providing a spectacular evidence for the coherent behaviour of these systems. In this experiment the two condensates were obtained by cutting a cigar-shaped atomic cloud into two separated parts with a laser beam. Clean fringes were observed in the overlapping region (see Figure 15.2) after expansion. A simple description of these fringes can be obtained by assuming that each condensate expands in an independent way. The time evolution of the phase S of each condensate is then easily calculated and for large times is described by the asymptotic law (see Section 12.7) S(r, t) →

1 mr2 . 2 t

(15.8)

0.12 mm

Figure 15.2 Interference fringes observed by imaging two Bose–Einstein condensed atomic clouds which overlap after expansion. From Andrews et al. (1997b). Reprinted by permission c 1997, American Association for the Advancement of Science. from Science, 275, 637;

Interference between two condensates

277

This result is independent of the initial form of the conﬁning potential and simply reﬂects the classical nature of the velocity ﬁeld v = (/m)∇S = r/t for large times. Let us now assume that, at t = 0, the order parameter is described by the linear combination Ψ(r) = Ψa (r) + eiΦ Ψb (r),

(15.9)

where Ψa and Ψb are the initial wave functions of the two condensates (hereafter called a and b) which are assumed to be real and separated in space: Ψ∗a (r)Ψb (r) 0

(15.10)

everywhere. Actually, the initial overlap between the two wave functions is not exactly zero, but is exponentially small if the distance d between the condensates is large enough. The value of Φ ﬁxes the relative phase of the two condensates at the initial time t = 0. For large times the relative phase between the two condensates approaches the value Φ + S(x, y, z + d/2)−S(x, y, z−d/2) = (md/t)z+Φ, where we have assumed that the condensates are aligned along the z-axis. When the two condensates overlap the total density n = |Ψ|2 exhibits modulations of the form md z+Φ , (15.11) n(r, t) = na (r, t) + nb (r, t) + 2 na (r, t)nb (r, t) cos t characterized by straight line fringes, orthogonal to the zth axis. In eqn (15.11) na,b (r, t) = |Ψa,b (r, t)|2 are the densities of the two expanding clouds. The spacing between two consecutive fringes is given by the simple expression λ=

ht , md

(15.12)

while their position is ﬁxed by the initial value of the relative phase. Notice that the amplitude of the crossed term in eqn (15.11) becomes comparable to the other terms for large times due to the spreading of the two wave functions Ψa,b . Using the spacing between the centres of the two initial condensates as an estimate of the distance d, one gets fringe periods in reasonable agreement with the patterns observed in the MIT experiment. Typical values are t 40ms, d 40μm, and λ 20μm. The geometry used in this experiment was not, however, the most suitable to apply the simple model described above since the initial separation between the condensates was too small to ignore interaction eﬀects between the overlapping clouds during the expansion. For a more quantitative analysis of this experiment it is consequently necessary to carry out a full numerical solution of the time-dependent Gross-Pitaevskii equation (R¨ ohrl et al., 1997). These calculations are in remarkable agreement with experiments (see Figure 15.3). A better geometry to emphasize the eﬀects of interference would be obtained by working with two parallel discs rather than with two aligned cigars. In this case the two condensates can be put very close each other, with the consequent increase of λ.

278

Coherence, Interference, and the Josephson Eﬀect 0.008

P(z)

(a) 0.004

0.000 P(z)

(b) 0.004

0.000 P(z)

(c) 0.004

0.000 –250

–125

0 z [μm]

125

250

Figure 15.3 Density pattern P (z) for the interference of two expanding and overlapping condensates. (a) Theory by R¨ ohrl et al. (1997) based on the solution of the time-dependent GP equation. (b) Experimental data by Andrews et al. (1997b). (c) Theory including the eﬀect of ﬁnite experimental resolution. Reprinted with permission from Physical Review Letters, 78, c 1997, American Physical Society. 4143;

If the condensates contain a vortex line the interference patterns exhibit interesting topological structures since the evolutions of the phase due to the expansion add in a non trivial way to the initial phase of the vortex (Tempere and Devreese, 1998; Bolda and Walls, 1998). For example, if the condensate b contains a vortex its order parameter, at t = 0, has the form Ψb = |Ψb |eiϕv , where ϕv is the azimuth angle (see eqn (14.29)). After expansion the two condensates overlap and the density proﬁle will have the same structure (15.11) with the replacement md md cos z + Φ → cos z + Φ + ϕv . (15.13) t t The corresponding structure of fringes exhibits dislocation patterns (see Figure 15.4) which have been observed experimentally by Inouye et al. (2001), and Chevy et al. (2001). The above discussion on interference raises the relevant question of what the shape of the measured proﬁle would be if the condensates, instead of being initially in the coherent conﬁguration (15.9), were independent with an undetermined value of the relative phase. It is useful to describe the problem employing the Fock representation

Interference between two condensates

279

20 10

y

0 −10 −20 −40

−20

0 x

20

40

Figure 15.4 Calculated interference patterns produced by two overlapping condensates in the presence of a vortical line. The dislocation of the interference fringes is clearly visible. From Bolda and Walls (1998). Reprinted with permission from Physical Review Letters, 81, c 1998, American Physical Society. 5477;

of the many-body wave function. In ﬁrst approximation, the independent conﬁguration is described by the choice |F = √

† Na † Nb 1 a |vac, b Na !Nb !

(15.14)

operators relative to hereafter called Fock state, where a ˆ√† and ˆb† are the creation √ the single-particle states φa = Ψa / Na and φb = Ψb / Nb , respectively, and |vac is the state vacuum of particles. The single-particle wave functions φa and φb are normalized to unity and are orthogonal at t = 0 due to the condition (15.10). The Fock conﬁguration was already employed in Section 15.1 to investigate the eﬀects of two-body interactions on the possible occurrence of Bose–Einstein fragmentation. Notice, however, that in that case the two wave functions were fully overlapping. It is worth noticing that the Fock state (15.14) is an exact eigenstate of the number ˆa = a ˆb = ˆb†ˆb. It actually corresponds to a conﬁguration with operators N ˆ† a ˆ and N fragmented Bose–Einstein condensation. The Fock state (15.14) should be compared with the ‘coherent’ conﬁguration † N 1 |Φ = √ a + e−iΦ b† |vac, (15.15) N N !2 which is instead √ obtained by putting all the N atoms in the same single-particle state ˆa,b on the state (15.15) is (φa + eiΦ φb )/ 2. The average value of the operators N ˆa,b . equal to N/2. However, in contrast to (15.14), this state is not an eigenstate of N Actually, by applying the binomial expansion to the operator (a† + e−iΦ b† )N one ﬁnds that the coherent conﬁguration corresponds to a linear combination of Fock states with diﬀerent values of Na and Nb |Φ = e−iN Φ/2 C(k)eikΦ |k, (15.16) k

280

Coherence, Interference, and the Josephson Eﬀect

where we have introduced the parameter k = (Na − Nb )/2 to label the Fock state with Na = N/2 + k and Nb = N/2 − k and the coeﬃcients √ N! C(k) = . (15.17) N 2 (N/2 + k)! (N/2 − k)! Using the Stirling formula for the factorial one can approximate C (k) ∝ exp(−k 2 /N ), yielding the result ˆa − N ˆb )2 |Φ − (Φ|(N ˆa − N ˆb )|Φ)2 = N Φ|(N

(15.18)

for the ﬂuctuations of the relative number of particles in the two wells. Notice that coherent states (15.15) with diﬀerent values of the phase are not exactly orthogonal, except in the large N limit. Let us now discuss the problem of the measurement of the relative phase between condensates which overlap after expansion, and let us assume that initially the system is described by the Fock conﬁguration (15.14) with Na = Nb = N/2. If one neglects the interaction between the two condensates, the Fock structure of the many-body wave function is preserved during the expansion until the measurement process takes place. Since the Fock state (15.14) can be written as a combination of the coherent states (15.15) according to |F =

1 2π

+π

−π

|Φ dΦ,

(15.19)

the measurement of the interference fringes, which gives access to the value of Φ, corresponds to a typical problem of reduction of the wave packet (Anderson, 1986). According to the general rules of quantum mechanics the measurement will provide a value of Φ ranging from −π to +π with equal probability and the system, after measurement, will be projected into the corresponding coherent conﬁguration (15.15). Each measurement of the interference patterns obtained starting from the initial state (15.14) will then provide a density proﬁle of the form (15.11). However, the relative phase Φ will be diﬀerent in diﬀerent measurements and the average value, obtained through several repetitions of the experiment, will give the incoherent sum n(r, t)F = |Ψa (r, t)|2 + |Ψb (r, t)|2 .

(15.20)

The situation diﬀers if instead the initial conﬁguration corresponds to a coherent state of the form (15.15) with a given value of Φ. In this case the value of the phase will always be the same in each repetition of the experiment. In order to observe interference eﬀects in the density proﬁle it is crucial that the two condensates Ψa and Ψb overlap in space, otherwise the third term in the right-hand side of eqn (15.11) would be identically zero. This does not mean, however, that the eﬀects of coherence cannot also be observed if the condensates are separated in space. In this case the good observable to consider is not the density, but the momentum distribution, a quantity which naturally emphasizes the eﬀects of non locality and

Interference between two condensates

281

long-range order. Let us consider the simplest case in which the external potential conﬁnes the two condensates in a symmetric way and the order parameters can be obtained by the simple translation: Ψa (r) = Ψb (r + d). This condition is not diﬃcult to achieve if the distance between the two condensates is large enough and implies that, in momentum space, the order parameters are simply related by the equation Ψa (p) = e−ipz d/ Ψb (p),

(15.21)

where Ψ(p) = (2π)−3/2 dre−ip·r/ Ψ(r). Equation (15.21) explicitly shows that, despite the fact that Ψa and Ψb are fully separated in coordinate space, their overlap in momentum space is complete, giving rise to visible interference eﬀects in the momentum distribution. In fact, using eqn (15.21), one immediately ﬁnds that the momentum distribution of the coherent conﬁguration is given by

pz d 2 n(p) = |Ψ(p)| = 2 1 + cos + Φ na (p), (15.22) where na (p) = nb (p) is the momentum distribution of each condensate. If one instead calculates the average momentum distributions using the Fock state (15.14), one ﬁnds the incoherent result n(p)F = na (p) + nb (p) = 2na (p).

(15.23)

The fringe structure exhibited by the momentum distribution (15.22) reﬂects the occurrence of an interesting behaviour in the one-body density matrix. By using relationship (2.5) and the Gaussian approximation (15.7) for the one-body density matrix of each condensate, one ﬁnds the result (we choose Φ = 0 for simplicity)

2 2 2 2 1 −(s+d)2z /2χ2 n(1) (0, 0, sz ) = N e−sz /2χ + e , (15.24) + e−(s−d)z /2χ 2 which explicitly shows that long-range order, which for a single condensate is characterized by the coherence length χ ∼ Rz , now extends up to larger values of the order of relative distance between the two condensates (see Figure 15.5). Measuring the momentum distribution is achievable, either by setting the scattering length equal to zero (proﬁting from the presence of a Feshbach resonance) just before the expansion, or using two-photon Bragg spectroscopy (see Section 12.8). The quantity actually measured in the latter case is the number of scattered atoms as a function of the energy transferred by the photon to the sample. This gives access to the dynamic structure factor, which can be related to n(p) if one works in the impulse approximation (IA) regime, where one can write m S(q, ω) = n(px , py , Y )dpy dpz . (15.25) q Here Y = (m/q)(ω − q 2 /2m) and q and ω are, respectively, the momentum and energy transferred by the photon to the condensate in each scattering event. The IA

282

Coherence, Interference, and the Josephson Eﬀect 1

n(1)(sz / d )

d = 6χ

0.5

0 −10

−5

0 sz / d

5

10

Figure 15.5 Oﬀ-diagonal one-body density matrix in arbitrary units for two separated condensates with relative phase Φ = 0. The width of each peak is ﬁxed by the size of each condensate. Coherence extends up to the distance d between the two condensates.

regime holds for high values of momentum transfer. Inserting result (15.22) for the momentum distribution into eqn (15.25) one ﬁnds the simple factorization (Pitaevskii and Stringari, 1999)

S(q, ω) = 2 1 + cos

dY + Φ Sa (q, ω),

(15.26)

hq characterized by frequency fringes with period Δω = md . In eqn (15.26) Sa (q, ω) = Sb (q, ω) is the value of the dynamic structure factor of each condensate. An advantage of interference measurements in momentum space is that they are not destructive. In fact, the Bragg scattered atoms which provide the measured signal are very energetic and can be detected without releasing the conﬁning traps. The phase diﬀerence between two condensates was measured by Saba et al. (2005). In this experiment an optical double-well trap was created by a laser beam, splitting the condensate into two parts. A diﬀerence between the chemical potentials of the two condensates was then produced with magnetic ﬁeld gradients, causing the time evolution of the phase diﬀerence according to (see eqn (6.18))

Φ = Φ0 + (μ2 − μ1 )t/.

(15.27)

Two laser beams of opposite directions and frequency diﬀerence matched to the recoil energy ω = q 2 /2m, corresponding to Y = 0 in eqn (15.26), were then applied to the condensates. For each scattered atom a photon was transferred from one beam to another and the intensity of scattering was determined in a continuous way by measuring the intensity of one of the two laser beams. In these experimental conditions

Interference between two condensates

283

the intensity of the signal is proportional to (1 + cos(Φ)) and consequently oscillates with the frequency (μ2 − μ1 )/ according to

(μ2 − μ1 ) t , (15.28) S(q, ω) ∝ 1 + cos Φ0 + allowing, in particular, for the measurement of the initial phase diﬀerence Φ0 . It is worth noticing that the interference signal takes place because the wave functions of the atoms outcoupled from the two condensates overlap in space. If the two condensates are initially independent, i. e. if they stay in the Fock state (15.14), the measurement would give a deﬁnite value of the phase diﬀerence. However, in diﬀerent realizations of the experiments these values are randomly distributed. Once measured, the phase diﬀerence evolves in time according to eqn (15.27). A further important demonstration of the coherent nature of Bose–Einstein condensates is the four-wave mixing experiment, where three diﬀerent de Broglie waves with atomic energies 1 , 2 , and 3 and momenta p1 , p2 , and p3 overlap to produce

Figure 15.6 Results of four-wave mixing of atomic de Broglie waves. Each peak represents atoms with diﬀerent momenta observed after a period of free ﬂight, which allows the diﬀerent components to separate. From Deng et al. (1999). Reprinted by permission from Nature, 398, c 1999, Macmillan Publishers Ltd. 218;

284

Coherence, Interference, and the Josephson Eﬀect

a fourth wave with energy 4 = 1 + 2 − 3 and momentum p4 = p1 + p2 − p3 (Deng et al., 1999). In this experiment the waves 1, 2, and 3 have been produced by two consecutive Bragg pulses generated by intersecting laser beams during the free expansion of a condensate of sodium atoms. These pulses create atoms in states 2 , p2 and 3 , p3 . The ﬁrst state is provided by the initial state with p1 = 0. The process of four-wave mixing is well known in nonlinear optics, where three electromagnetic waves produce the polarization of the medium which radiates the fourth wave. While in nonlinear optics the process is due to the nonlinear properties of the medium, four-wave mixing in atomic systems exists due to the interatomic force, responsible for the nonlinear term in the GP equation. Retaining the nonlinear term, namely the contribution proportional to e−i4 t/ , the equation for Ψ4 can be written as

∂ 2 2 i + ∇ Ψ4 = 2gΨ1 Ψ2 Ψ∗3 . ∂t 2m

(15.29)

Analogous equations can be derived for Ψ1 , Ψ2 , and Ψ∗3 . These equations describe the coherent creation of the fourth wave and the ampliﬁcation of the original wave Ψ3 , while the waves Ψ1 and Ψ2 are consequently attenuated. The diﬀerent momentum components of the condensate move with diﬀerent velocities and eventually separate, as illustrated in Figure 15.6.

15.3

Double-well potential and the Josephson eﬀect

The Josephson eﬀect is an important quantum phenomenon ﬁrst discovered in superconductors and later in superﬂuid helium (for a general review see, for example, Barone and Paterno, 1982). It consists of a coherent ﬂow of particles which tunnel through a barrier in the presence of a chemical potential gradient. The possibility of observing similar eﬀects in trapped Bose–Einstein condensates represents a challenging perspective in the study of coherence phenomena in quantum gases (see, for example, Leggett, 2001). We start our investigation by developing the formalism in the framework of mean-ﬁeld theory. We will see, however, that important deviations from the mean-ﬁeld picture can take place under suitable conditions of great physical interest. Let us consider a gas of atoms conﬁned by two wells separated in the z-direction and let us assume that the trapping potential is symmetric with respect to the centre of the barrier: Vext (x, y, z) = Vext (x, y, −z) (see Figure 15.7). We can naturally construct an approximate solution of the Gross-Pitaevskii equation for this potential if we assume that the overlap between the two condensates is small. The ﬁrst step is to ﬁnd a solution describing the wave function within each well. This can be obtained by solving the Gross-Pitaevskii equation for Na atoms localized in the well a. Analogously, one can solve the same equation for Nb atoms localized in the well b. The corresponding functions Ψa,b can always be chosen to be real and to satisfy the normalization condition Ψ2a,b dr = Na,b . Their shape depends explicitly on the number of atoms Na,b because of the presence of two-body interactions in the Hamiltonian.

Double-well potential and the Josephson eﬀect

285

The ground state solution of the problem containing N = Na + Nb atoms is given by the symmetric combination

N N (15.30) + Ψb r, e−iμt/ , Ψ (r,t) = Ψa r, 2 2 where N is the total number of atoms and μ is the chemical potential. By writing (15.30) we have explicitly used the fact that, in the region inside the barrier, where the functions Ψa and Ψb overlap, the system is very dilute and the GP equation reduces to a linear Schr¨ odinger equation. Thus (15.30), within proper accuracy, is a solution of the Gross-Pitaevskii equation everywhere. The symmetric conﬁguration corresponds to the ground state since it minimizes the kinetic energy in the overlapping region. If the overlap becomes large then the solution cannot simply be written in the form (15.30) and the ground state solution should be found by directly solving the full GP equation. Solving the Gross-Pitaevskii equation numerically can provide a practical way to determine the wave functions Ψa and Ψb . One ﬁrst calculates the lowest symmetric (Ψgs ) and antisymmetric (Ψex ) solutions and then takes the linear √ combinations Ψa,b = (Ψgs ± Ψex )/ 2. Notice that according to this prescription the wavefunctions Ψa,b are automatically orthogonal. If the distance between the wells or the height of the barrier is suﬃciently large the overlap between the wavefunctions Ψa,b will be exponentially small. Using a similar procedure one can derive nonstationary solutions of the timedependent Gross-Pitaevskii equation describing the exchange of atoms between the two wells. These solutions can be conveniently presented in the form Ψ (r,t) = Ψa (r, Na ) eiSa + Ψb (r, Nb ) eiSb , (15.31) where Na , Nb and Sa , Sb are functions of time. The total number of particles N = Na + Nb is of course a constant of motion.

Vext

μb

μa

a

−20

−10

b

0 z

10

20

Figure 15.7 Schematic picture of a double-well potential trapping two Bose–Einstein condensates.

286

Coherence, Interference, and the Josephson Eﬀect

An important feature exhibited by the wave function (15.31) is the occurrence of an atomic current I = ∂Na /∂t = −∂Nb /∂t between the two wells if the relative phase Φ = Sb − Sa does not vanish. The current, calculated at z = 0, takes the simple expression (Josephson, 1962) I = −IJ sin Φ, with the amplitude deﬁned by

∂Ψb ∂Ψa dxdy Ψa − Ψb . IJ = m ∂z ∂z z = 0

(15.32)

(15.33)

The Josephson amplitude IJ is a positive quantity since, inside the barrier, the function Ψb increases while Ψa decreases with z. In order to obtain the equation for the relative phase Φ we recall that the time dependence of the phase of the order parameter is in general deﬁned by eqn (6.18), namely

m ∂S =− vs2 + μ . ∂t 2

(15.34)

Since the superﬂuid velocity created by the Josephson current is always small, one can neglect the term in vs2 and the equation for Φ takes the simple form ∂Φ 1 = − (μb − μa ), ∂t

(15.35)

where μa and μb are the chemical potentials relative to the condensates in the two wells. In the following the deviations of Na and Nb from their equilibrium value N/2 will be assumed to be small, so that, by introducing the relevant variable k = (Na − Nb ) /2 , |k| N,

(15.36)

ﬁxed by the diﬀerence between the numbers of atoms in the two wells, and expanding the chemical potentials with respect to k, we can rewrite eqn (15.35) as EC ∂Φ = k, ∂t

(15.37)

dμa dNa

(15.38)

where EC = 2

is the relevant interaction parameter of the problem calculated at Na = Nb = N/2. Analogously, eqn (15.32) for the current can be rewritten as ∂k = −IJ sin Φ, ∂t

(15.39)

Double-well potential and the Josephson eﬀect

287

where the current amplitude (15.33) should also be calculated setting Na = Nb = N/2. The value of EC vanishes by deﬁnition in the noninteracting gas since in this case the chemical potential of the two condensates does not depend on N . Instead in the Thomas–Fermi limit the coupling constant EC takes the value EC = (4/5)μa /Na ∝ N −3/5 , which follows from the N 2/5 dependence of the chemical potential (see eqn (11.8)). In the Thomas–Fermi regime the value of EC hence decreases with N . The Josephson amplitude IJ instead increases with N . In the Thomas–Fermi limit the amplitude IJ can be calculated using semiclassical approaches (Dalfovo et al., 1996; Zapata et al., 1998). Equations (15.37) and (15.39) coincide with the classical equations of the pendulum. Their solutions have diﬀerent forms depending on the initial conditions. If k and Φ are suﬃciently small, the equations can be linearized and describe a simple harmonic oscillation with frequency √ ωpl =

EC EJ ,

(15.40)

also called the plasma frequency, where we have introduced the Josephson energy EJ = IJ . Equation (15.40) gives the frequency of the classical oscillation of the condensate between the two wells. For initial values of |k| larger than 2EJ /EC the solutions of the classical equations (15.37) and (15.39) instead correspond to a full rotation of the phase while the relative number of atoms is approximately constant. If |k| is much larger than 2EJ /EC the phase evolves according to the law Φ = tEC k0 / and k exhibits small-amplitude oscillations EJ k = k0 1 + cos(E k t/) C 0 EC k02

(15.41)

around the average value k0 . Due to the condition |k| N this scenario is possible only if N 2 EC /EJ 1. The applicability of the above results requires that the tunnelling probability through the barrier is small enough. In fact, in order to decouple the Josephson motion from the internal oscillations of the condensate, the quantities Φ and k should vary slowly in time with respect the oscillator time 1/ωho . Using result (15.40) for the Josephson frequency this implies the condition

EJ EC ωho .

(15.42)

Experiments with a condensate in the two-well Josephson conﬁguration discussed above were performed by Albiez et al. (2005). These authors observed plasma oscillations at relatively small population imbalance k and self-trapping with the rotation of the phase when the imbalance is larger (see Figure 15.8). The Josephson eﬀect in a Bose–Einstein condensate was also investigated experimentally by Levy et al. (2007).

288

Coherence, Interference, and the Josephson Eﬀect (a) Josephson oscillations

(b) Self-trapping

4.4 μm 0 ms

5 ms

10 ms

15 ms

20 ms

25 ms

30 ms

35 ms

40 ms

45 ms

50 ms

Figure 15.8 Observation of the tunnelling dynamics of two weakly linked Bose–Einstein condensates in a symmetric double-well potential as indicated in the schematics. The time evolution of the population of the left and right potential well is directly visible in the absorption images. (a) Josephson oscillations are observed when the initial population diﬀerence is chosen to be below a critical value. (b) In the case of an initial population diﬀerence greater than the critical value the population in the potential minima is nearly stationary (selftrapping). From Albiez et al. (2005). Reprinted with permission of Physical Review Letters, c 2005, American Physical Society. 95, 010402;

Double-well potential and the Josephson eﬀect

289

The Josephson eqns (15.37) and (15.39) can be rewritten in the useful Hamiltonian form ∂Φ ∂HJ = ∂t ∂ (k)

(15.43)

∂HJ ∂ (k) =− , ∂t ∂Φ

(15.44)

and

respectively, which permits us to identify Φ and k as the natural canonically conjugated variables of the problem. The equations of motion are governed by the Josephson Hamiltonian (see, for example, Zapata et al. 1998): HJ = EC

k2 − EJ cos Φ . 2

(15.45)

In deriving the eqn (15.39) for the current we have evaluated the Josephson amplitude by setting Na = Nb in (15.33). This is an approximation since the wave functions Ψa,b depend on the number of atoms Na,b , and an explicit dependence on k should consequently emerge from the amplitude of the Josephson current. By writing the order parameters in the form Ψa,b = Na,b φa,b , with φa,b normalized to unity, one ﬁnds that the Josephson energy EJ = IJ will exhibit an additional dependence on the relative number k = (Na − Nb )/2 according to EJ = where we have used

√

δJ 2 N − 4k 2 , 2

√ N 2 − 4k 2 /2 and we have deﬁned

2 ∂φb ∂φa dxdy φa − φb δJ = . m ∂z ∂z z = 0

(15.46)

Na Nb =

(15.47)

In the limit of an almost ideal gas (EC → 0), eqn (15.46) exploits the whole dependence of EJ on Na,b . In fact, in this case the value of δJ is independent of Na,b since the wave functions φa,b are completely determined by the external potential. In this limit the quantity δJ coincides with the energy level splitting in the double well due to the tunnelling through the barrier (see eqn (15.86) below). The energy of the system, apart from a constant term, is then ﬁnally given by HJ = E C

k2 δJ 2 − N − 4k 2 cos Φ . 2 2

(15.48)

The correction in k 2 contained in (15.48) becomes crucial if the parameter EC is smaller than δJ /N . In fact, in this limit it provides the main k dependence of the Hamiltonian. The dynamic behaviour of two trapped Bose–Einstein condensates, based on the Hamiltonian (15.48), has been investigated by Smerzi et al. (1997) and Raghavan et al. (1999).

290

Coherence, Interference, and the Josephson Eﬀect

In the limit of small oscillations around equilibrium (Φ = 0, k = 0) the Hamiltonian (15.48) takes the form HJ = −

2 N δJ 2 N δJ δJ k + Φ + 2 + EC , 2 4 N 2

giving rise to Josephson oscillations with frequency 1 N EC . ωJ = δJ δJ + 2

(15.49)

(15.50)

If δJ N EC (hereafter called Josephson regime) one recovers the plasma frequency (15.40). In the opposite limit (hereafter called Rabi regime) δJ N EC ωJ instead coincides with the Rabi frequency δJ /. The system described by the Hamiltonian (15.48) exhibits diﬀerent scenarios that can be explored by writing the equations of motion (15.43) and (15.44) in the form (Smerzi et al., 1997 and Raghavan et al., 1999) z(t) ˙ = − 1 − z 2 (t) sin Φ δJ

(15.51)

z(t) ˙ Φ(t) = Λz(t) + cos Φ, δJ 1 − z 2 (t)

(15.52)

and

where z = 2k/N and Λ = N EC /2δJ . If Λ < 1, the system has two equilibrium solutions at k = 0 and Φ = 0 , π. The resulting phase trajectories in the k–Φ plane are closed lines around these two points, corresponding to periodic oscillations, and are separated by a separatrix. If 1 < Λ < 2, there are instead three equilibrium solutions: one at Φ = 0, k = 0 and two at Φ = π, k = ±(N/2) 1 − (1/Λ2 ). Finally, if Λ > 2, there is one stable solution at Φ = 0, k = 0. The closed trajectories around this point are separated by a separatrix from the rotating phase trajectories at large |k| (self-trapping solutions). The three regimes discussed above were experimentally observed by Zibold et al. (2010). These authors actually considered condensates which are not spatially separated, but occupy diﬀerent internal hyperﬁne states. The corresponding oscillations, giving rise to the so-called internal Josephson eﬀect, will be discussed in Section 21.3.

15.4

Quantization of the Josephson equations

The equations for the Josephson dynamics derived in the previous section correspond to the classical description of the oscillations of a Bose gas developed in Sections 5.6 and 12.2 in the framework of Gross-Pitaevskii theory. In dilute gases the quantization of the classical oscillations usually gives rise to small corrections, like the quantum

Quantization of the Josephson equations

291

depletion of the condensate, which do not change the behaviour of the system in a signiﬁcant way. In this section we will show that the eﬀects associated with the quantization of the Josephson equations can instead result in qualitatively new phenomena due to the ﬂuctuations of the phase originating from the overlapping region. These ﬂuctuations become increasingly large as the overlap between the two wave functions is reduced and eventually destroy the coherence of the ground state. This should be contrasted with the opposite behaviour taking place in the presence of a strong overlap where BEC is reinforced by the presence of repulsive forces (see Section 15.1). In order to quantize the classical equations (15.43)–(15.45) one has to replace the conjugated variables Φ and k with operators satisfying the commutation relation ˆ = i. Hence one has ˆ k] [Φ, ˆ = i. ˆ k] [Φ,

(15.53)

It is often convenient to work in the ‘Φ representation’, where ∂ kˆ = −i , ∂Φ

(15.54)

so that our system can be described by the Hamiltonian 2 ˆ J = − EC ∂ − EJ cos Φ H 2 ∂Φ2

(15.55)

acting in the space of the periodical functions of Φ with period 2π. Alternatively, one can use the ‘k representation’, where the phase can be written as ˆ =i ∂ . Φ ∂k

(15.56)

One should not forget that the quantization procedure presented above is approximate. In fact, the eigenvalues of the operator kˆ are all the integer numbers but, by construction, these values should always satisfy the condition |k| ≤ N/2. This implies that the Hamiltonian (15.55) describes in a correct way only states with values of |k| signiﬁcantly smaller than N. Furthermore, the use of the Hamiltonian (15.55) is justiﬁed only if the condition δJ N EC is satisﬁed (see the discussion at the end of the previous section). Because of the periodicity constraint, the uncertainty relation obeyed by the ﬂucˆ ad kˆ takes the form (for sake of simplicity in the following tuations of the observables Φ we will omit the ‘hat’ in these operators) * 2+ * + Δk Δ sin2 (Φ − Φ0 ) ≥ cos(Φ − Φ0 )2 /4 (15.57) holding for any value of the phase Φ0 , and where * + ΔA2 = A2 − A2

(15.58)

292

Coherence, Interference, and the Josephson Eﬀect

is the usual variance of the observable A. The inequality (15.57) has the same form as the uncertainty relation holding for the angular momentum and angle operators (Carruthers and Nieto, 1968). Only if the value of the phase is localized * +around * + Φ = Φ0 will the uncertainty relation (15.57) reduce to the usual form Δk 2 ΔΦ2 ≥ 1/4. The quantity α = cos(Φ − Φ0 )

(15.59)

characterizing the right-hand side of eqn (15.57) has an important physical meaning. It provides the degree of phase coherence of the conﬁguration and will be called the coherence factor. If the value of the phase is localized around Φ0 , then the value of α is close to unity (full coherence). In this case one can expand eqn (15.59) and calculate the quadratic ﬂuctuations of the phase as * + ΔΦ2 = 2 (1 − α). (15.60) If instead the phase is delocalized and all its values are equally probable, then the value of α is zero (absence of coherence). The coherence factor α is directly related to the visibility of fringes in the interference patterns. This is best illustrated by the behaviour of the momentum distribution of two separate condensates. In the presence of coherence, corresponding to small ﬂuctuations of the phase, the value of n(p) exhibits clear interference fringes, as shown by eqn (15.22). If instead the relative phase exhibits ﬂuctuations then the ‘average’ behaviour of the interference patterns will exhibit a reduced visibility according to the equation

pz d n (p) = 2 1 + V cos + Φ0 na (p), (15.61) where na (p) = nb (p) is the momentum distribution corresponding to each separate condensate, V is the visibility factor (V ≤ 1), and the average is taken over several repetitions of the experiment. Simple considerations permit us to relate the parameter V to the coherence factor α. In fact, if in a single run of the experiment one measures the momentum distribution (15.22) with a given value of Φ, the average value of n(p) can be written in the form

pz d n (p) = 2 1 + cos(Φ − Φ0 ) cos + Φ0 (15.62) pz d + Φ0 na (p). − sin(Φ − Φ0 ) sin By using the condition sin(Φ − Φ0 ) = 0 as a criterion to deﬁne the phase Φ0 , we ﬁnd that the visibility V coincides with the coherence factor (15.59). In the classical limit the energy (15.45) is minimized by setting Φ = k = 0. The use of the quantum Hamiltonian (15.55) results in the occurrence of ﬂuctuations which can signiﬁcantly modify the classical behaviour. These ﬂuctuations depend on the combination EC /EJ of the parameters of the Josephson Hamiltonian (15.55). It is useful to

Quantization of the Josephson equations

293

recall that the ratio EC /EJ becomes increasingly large when the height of the barrier increases or the number of atoms decreases. Let us ﬁrst consider the case of strong tunnelling: EC 1 EJ

(15.63)

In this case the system undergoes small oscillations around the equilibrium value Φ = 0 and consequently one can expand the Hamiltonian as 2 2 ˆ J = − EC ∂ + EJ Φ − EJ . H 2 2 ∂Φ 2

(15.64)

√ This corresponds to a traditional harmonic oscillator with frequency ωpl = EC EJ /. The phase ﬂuctuations exhibited by the ground state of (15.64) obey the relation * + 1 EC ΔΦ2 = 1 (15.65) 2 EJ and are, as expected, small. One can consequently regard eqn (15.63) as the physical condition for applying the classical Gross-Pitaevskii theory to the problem of the double-well potential. The ﬂuctuations of k in the ground state of the Hamiltonian (15.64) can also be calculated and one ﬁnds * 2+ 1 EJ 1 Δk = = 1. (15.66) 4 ΔΦ2 2 EC In limit the uncertainty relation (15.57) reduces the usual form * the + *strong-tunnelling + Δk 2 ΔΦ2 ≥ 1/4 and actually becomes an identity in the ground state (see eqns (15.65) and (15.66)) as a consequence of the harmonic nature of + the Hamiltonian. * Notice, however, that in the limit of very small Ec , when ΔΦ2 is of the order of 1/N , the expression (15.55) for the Hamiltonian is no longer adequate and one should instead use the Hamiltonian (15.48). In this case even the physical interpretation of the phase operator and of the coherence factor (15.59) should be revisited (see Section 15.7). In the opposite Fock case of weak tunnelling: EC 1, EJ

(15.67)

the behaviour of the eigenvalues of the Hamiltonian and of the ﬂuctuations is very diﬀerent. The Josephson term EJ entering the Hamiltonian (15.55) can be neglected in ﬁrst approximation and the Hamiltonian takes the form −(EC /2)∂ 2 /∂Φ2 , whose eigenstates are plane waves einΦ for integer values n. The ground state wave function in the ‘Φ representation’ is then a constant, revealing that the relative phases between the two condensates is distributed in a random way. The energy of the ﬁrst excited state is simply given by EC /2. From the many-body point of view the ground state of

294

Coherence, Interference, and the Josephson Eﬀect

the system in the weak tunnelling limit corresponds to the Fock conﬁguration (15.14) already discussed in Section 15.2. The ﬁrst corrections due to the Josephson term −EJ cos Φ can be obtained by applying perturbation theory. The ground state wave function of the Hamiltonian (15.55) is no longer constant, but is proportional to 1 + 2(EJ /EC ) cos Φ. In the same limit one ﬁnds α=2

EJ , EC

(15.68)

while the ﬂuctuations of the relative number of particles takes the value *

Δk

2

+

=2

EJ EC

2 (15.69)

and vanishes with the square of the tunnelling probability EJ . Similar to the case of the strong-tunnelling regime, in the weak tunnelling regime the uncertainty relation (15.57) also reduces to an identity. In Figure 15.9 we plot the coherence factor α as a function of the ratio EC /EJ , calculated by explicitly solving the Schr¨ odinger equation with the Josephson Hamiltonian (15.55). The ﬁgure shows that for values of EJ smaller than EC the degree of coherence is signiﬁcantly quenched, illustrating the occurrence of the transition to the Fock regime.

1 0.9 0.8 0.7

α

0.6 0.5 0.4 0.3 0.2 0.1

0

2

4

6

8

10

EC /EJ

Figure 15.9 Coherence factor (15.59), calculated in the double-well potential at T = 0, as a function of the ratio EC /EJ (see text). From Pitaevskii and Stringari (2001).

Quantization of the Josephson equations

295

The results derived in this section hold in an ideal situation of zero temperature. This implies that the system is not excited during its preparation. If, for example, the Josephson conﬁguration is created by cutting the condensate into two parts by increasing the height of the barrier, this ramping should be produced adiabatically, over times longer than the time 1/ωJ ﬁxed by the frequency of the Josephson oscillation (Leggett and Sols, 1998; Menotti et al., 2001). Thermal eﬀects should also be taken into account. In principle, due to the smallness of the coupling constants of the Josephson Hamiltonian, the thermal ﬂuctuations of the phase can become important, even at very low T . In fact, the relevant scale of temperature is provided by the energy ωJ , which, because of the constraint (15.42), corresponds to extremely small values of T . So, the thermal ﬂuctuations of the phase can easily destroy the coherence of the Josephson conﬁguration (Pitaevskii and Stringari, 2001). To investigate the thermal eﬀect, one should calculate the thermal average of the visibility α, deﬁned according to (15.59). The theory is particularly simple in the high temperature limit kB T ωJ . Then only the second term in the Hamiltonian (15.55) is important and one can use the classical equation +π EJ EJ cos Φ I dΦ cos Φ exp 1 −π kB T kB T , αcl (T ) = = (15.70) +π EJ EJ cos Φ dΦ exp I0 −π kB T kB T where I0,1 are the modiﬁed Bessel functions of the ﬁrst kind. The thermal phase ﬂuctuations of a condensate in the Josephson conﬁguration were investigated by Gati et al. (2006), using double-well conﬁgurations. The measurements qualitatively conﬁrmed the prediction (15.70) for the visibility. One should not, however, forget that the hypothesis of thermal equilibrium is by no means obvious in the Josephson conﬁguration, since the relaxation times needed to ensure thermal equilibrium between samples separated by a high barrier can be extremely long. In conclusion, we have shown that, depending on the value of the parameters entering the Josephson Hamiltonian, the ground state of a dilute Bose gas conﬁned by a double-well potential can exhibit very diﬀerent conﬁgurations, ranging from the coherent state described by Gross-Pitaevskii theory to the Fock state where the two trapped gases have, separately, a well-deﬁned number of atoms but a random relative phase. The latter conﬁguration is often called ‘number-squeezed’. The possibility of exploring regimes which are diﬀerent from the coherent one opens interesting perspectives in the study of new quantum phases. In this context it is worth remembering that the scenarios discussed so far refer to gases interacting with repulsive forces (a > 0). In the case of negative scattering lengths diﬀerent situations take place. In fact, while in the weakly interacting limit the ground state is still given by the coherent state (15.15), in the opposite limit the ground state corresponds to a ‘Schr¨ odinger cat’ (Ho and Ciobanu, 2000) whose leading component, in the Fock representation, has the form 1 |S = √ 2

1 1 √ (ˆ a† )N + √ (ˆb† )N N! N!

|vac,

(15.71)

296

Coherence, Interference, and the Josephson Eﬀect

reﬂecting the intrinsic tendency of the gas to collapse into the conﬁguration of highest density. The state (15.71) correspond to the linear combination of two macroscopic states and diﬀers signiﬁcantly from both the coherent and Fock conﬁgurations (15.15) and (15.14), respectively, previously considered. Of course ‘Schr¨ odinger cats’ of this type can only be produced if the value of N does not exceed the critical value ﬁxed by the relation (11.52).

15.5

Decoherence and phase spreading

In this section we address the question of the decoherence of the relative phase of two condensates. Dephasing can have either a quantum or a thermal origin. In the following we will consider the ideal situation of a system at zero temperature consisting of two condensates conﬁned in two separate wells. In the Fock representation the many-body wave function |Ψ(t = 0 at the time t = 0 can be written in the form |Ψ(0) = C (k) |k, (15.72) k

ˆa − N ˆb )/2. If where k and |k are eigenvalues and eigenstates of the operator kˆ = (N |Ψ(0) is the ground state of the many-body Hamiltonian then the time evolution * + of 2 this state is simply given by exp(−iE t/) and the ﬂuctuations of the phase ΔΦ = 0 −∂ 2 /∂k 2 = − C ∗ ∂ 2 C (k) /∂k2 dk remain constant in time. If instead |Ψ(t = 0 does not correspond to the ground state then the coherence properties will evolve in time. In general, this evolution cannot be described in a simple way. However, if we make the assumption that for t > 0 the Josephson coupling between the two condensates can be completely ignored, then the time-dependent solution is derived in an easy form. This assumption may correspond to a situation where we suddenly ramp up a high barrier separating the two condensates, causing the sudden vanishing of the Josephson coupling EJ , or to a situation where we consider two fully separated condensates which are prepared, at some time t = 0, in a coherent conﬁguration. Under the above hypothesis the time evolution of each Fock component | k is simply ﬁxed by the phase factor exp[−iE(k)t/], where E(k) = E(Na ) + E(Nb ) is the sum of the energies of the two condensates and Na,b = N/2 ± k. By assuming that only small values k = (Na − Nb )/2 are physically relevant one can easily expand 1 E(k) = E0 + EC k 2 , 2

(15.73)

where E0 is the energy of the system corresponding to k = 0 and EC = 2∂μa /∂Na = 2∂μb /∂Nb . The time dependence of the many-body state can be now simply derived and one obtains the result

1 −iE0 t/ 2 |Ψ(t) = e C(k) exp −i EC k t/ |k, (15.74) 2 k

showing that each Fock component evolves in time with its own phase, giving rise to a dispersion of the wave packet. Notice that this dispersion is a consequence of two-body interactions, since in the ideal gas one would have EC = 0.

Boson Hubbard Hamiltonian

297

The time evolution of the phase ﬂuctuations is then easily calculated and one ﬁnds the result ΔΦ2 t = ΔΦ2 0 + Δk 2

EC t 2

2 ,

(15.75)

where Δk 2 is the ﬂuctuation of the relative number of atoms, a quantity which, according to (15.74), is conserved in time. Result (15.75) reveals that phase coherence is lost after a time τ ﬁxed by the relation (Castin and Dalibard, 1997; see also Lewenstein and You, 1996; Wright et al. 1996) 1 1 EC = Δk. τ 2

(15.76)

Result (15.75) has been derived by replacing the sum over k in (15.74) with an integration. For large times, however, the discretized nature of the variable k is important. As a result, the coherence will be periodically restored with the revival time tr =

2π . EC

(15.77)

Indeed, for such a value of t the exponential factor in (15.74) becomes equal to exp[−iπ 2 k 2 ] = ±1, where the sign + (−) corresponds to even (odd) values of k. The comparison with eqn (15.16), which gives the general form of a coherent wave function characterized by the relative phase Φ, shows that after the revival time (15.77) the system will be found again in a coherent conﬁguration with a change of π in the relative phase.

15.6

Boson Hubbard Hamiltonian

In Sections 15.3–15.4 we described the properties of the Josephson Hamiltonian (15.55) and of its solutions in the important limits of weak and strong tunnelling. This discussion does not exhaust, however, all the relevant regimes. Actually, we have already pointed out that when the interaction coupling EC tends to zero even the classical description of the Josephson oscillation should include the additional k-dependent term in the Josephson energy (15.46). In the harmonic limit the new Hamiltonian reduces to eqn (15.48), giving rise to result (15.49) for the Josephson frequency. The quantum description in this regime requires a careful discussion, especially regarding the physical meaning of the phase operator. The problem emerges clearly in the simplest limit of the noninteracting where the quantization of the Hamiltonian √ gas (EC = 0), √ (15.48) yields the value < ΔΦ2 > = 1/ N for the ﬂuctuations of the phase. This seems to contradict the fact that, in the absence of two-body interactions, the ground state should correspond to the coherent state (15.15) with Φ = 0, resulting in a perfect visibility (V = 1) of the interference fringes. The quantum description of the system in the quasi-ideal regime is best understood using the formalism of the boson Hubbard Hamiltonian (Fisher et al., 1989;

298

Coherence, Interference, and the Josephson Eﬀect

Javanainen and Ivanov, 1999; Paraoanu et al., 2001). In the problem of the double well the Hamiltonian is simply derived using the representation ˆ Ψ(r) = φa (r)ˆ a + φb (r)ˆb

(15.78)

for the ﬁeld operator, where φa,b are the ground state single-particle wave functions generated by the external potential in the two separate traps, and by retaining the leading terms in the many-body Hamiltonian ˆ = H

2 2 ∇ g † ˆ ˆ †Ψ ˆ ˆ †Ψ ˆ Ψ. ˆ drΨ − + Vext Ψ + drΨ 2m 2

(15.79)

The explicit equations for the single-particle functions φa,b will be derived below (see eqns (15.84) and (15.85)). With the ansatz (15.78) we are excluding all the conﬁgurations of the condensate involving single-particle states diﬀerent from φa,b and their linear combinations. This is a good approximation if the resulting frequencies are small compared to the ‘internal’ frequencies which characterize the oscillations of the condensates within each trap. By assuming almost full separation between the two wells (tight binding approximation), the relevant terms of the Hamiltonian take the typical boson Hubbard form δ J ˆ BH = EC a H ˆ† a a ˆ†ˆb + ˆb† a ˆ† a ˆa ˆ + ˆb†ˆb†ˆbˆb − ˆ , 4 2

(15.80)

where φ4a dr

(15.81)

2 2 ∇ + Vext (r) φb (r). drφa (r) − 2m

(15.82)

EC = 2g and δJ = −2

In the considered limit of a weakly interacting gas, where the single-particle wave functions φa,b are not aﬀected by the presence of interactions, the above deﬁnitions of EC and δJ coincide with the values (15.38) and (15.47) introduced in Section 15.3. In order to discuss this quasi-ideal regime it is useful to calculate explicitly the unperturbed single-particle levels generated by the double-well trapping potential. These are provided by the solutions of the Schr¨ odinger equation 2 2 ∇ − + Vext (r) − ε φ(r) = 0. 2m

(15.83)

If one neglects the tunnelling through the barrier then this level has double degeneracy. The inclusion of tunnelling removes the degeneracy, giving rise to two diﬀerent levels ε0

Boson Hubbard Hamiltonian

299

and ε1 whose wave functions φ0 and φ1 are, respectively, symmetric and antisymmetric with respect to z = 0 and satisfy the Schr¨ odinger equations 2 2 2 2 ∇ ∇ − + Vext − ε0 φ0 (r) = 0, − + Vext − ε1 φ1 (r) = 0. (15.84) 2m 2m The wave functions φ0 and φ1 are normalized to unity. The lowest level (ground state) is given by the symmetric solution. Starting from these solutions one can construct the wave functions φa and φb localized in the two separate wells, through the relations 1 1 (φa + φb ) , φ1 = (φa − φb ), (15.85) φ0 = 2 2 which preserve the orthogonality relations. By expressing φa,b in terms of φ0,1 and using eqns (15.84) we now calculate the Josephson parameter (15.82), for which we ﬁnd the important relationship δJ = ε1 − ε0 .

(15.86)

Since, in the quasi-ideal regime, quantum ﬂuctuations provide only perturbative corrections, the boson Hubbard Hamiltonian can be diagonalized by developing the formalism of the Bogoliubov transformations (for a diﬀerent approach, see Franzosi et al., 2000). The calculation is similar to the one developed in Chapter 4. The ﬁrst step is to express the Hamiltonian (15.80) in terms of the particle operators a ˆ0 and ˆ and ˆb by the a ˆ1 relative to single-particle wave functions φ0 and φ1 , and related to a linear transformation 1 1 a ˆ0 = √ (ˆ a + ˆb), a ˆ1 = √ (ˆ a − ˆb). (15.87) 2 2 √ One then makes the prescription a ˆ0 → N , which corresponds to assuming that most of the atoms are Bose–Einstein condensed in the lowest state φ0 . By keeping terms ˆ1 and using the relation a ˆ†0 a ˆ0 +ˆ a†1 a ˆ1 = N to evaluate quadratic in the operators a ˆ0 and a the various terms of the Hamiltonian with proper accuracy, one ﬁnds that the boson Hubbard Hamiltonian can be written as EC †2 ˆ = δJ a H N a ˆ1 + a (15.88) ˆ†1 a ˆ1 + ˆ21 + 2ˆ a†1 a ˆ1 , 8 where we have omitted an unimportant constant term. Equation (15.88) is diagonalized by the Bogoliubov transformation a ˆ1 = uα ˆ + vα ˆ†, a ˆ†1 = uˆ α† + v α, ˆ

(15.89)

where the real amplitudes u and v are given by u, v = ±

δJ + N EC /4 1 ± 2εJ 2

1/2 (15.90)

300

Coherence, Interference, and the Josephson Eﬀect

and satisfy the normalization condition u2 −v2 = 1. The energy εJ entering eqn (15.90) is given by εJ =

δJ

N EC δJ + 2

(15.91)

and coincides with the classical result (15.50). In terms of the new quasi-particle operators α, ˆ α ˆ † , the Hamiltonian takes the diagonalized form ˆ† α ˆ + constant, H = εJ α

(15.92)

which can be used to investigate the quantum ﬂuctuations in the ground state. For example, the quantum depletion of the condensate, associated with the partial occupation of the state φ1 , is simply given by: δN0 = v 2 =

δJ + N EC /4 1 − . 2εJ 2

(15.93)

We can then verify that the condition of applicability of the Bogoliubov description (δN0 N ) requires the condition EC N δJ = 2EJ . This is compatible not only with the regime EC δJ /N, where the gas becomes ideal (v = 0), but also with the opposite regime EC δJ /N , where the k dependence in the Josephson parameter EJ can be safely neglected and one jumps into the strong-tunnelling regime discussed in Section 15.4. In this case the quantum depletion takes the form δN0 /N = EC /EJ /8. The above discussion proves that all the relevant regimes of the problem, corresponding to diﬀerent choices for EJ and EC , can be described with safe accuracy. Let us now discuss the behaviour of the visibility of interference fringes in the ˆ momentum distribution. Using the momentum representation Ψ(p) = φa (p)ˆ a +φb (p)ˆb of the ﬁeld operator (15.78) one can evaluate the average value of the momentum ˆ † (p)Ψ(p). ˆ distribution n(p) = Ψ If we approximate φa (r) φb (r + d), where |d| is the distance between the two wells, one has φa (p) = e−ipz d/ φb (p) and the momentum distribution takes the form

a† b + b† a cos n(p) = 1 + N

pz d

a† b − b† a +i sin (px d) na (p), N

(15.94)

where na (p) = Na |φa (p)|2 = nb (p) is the momentum distribution of each condensate. Taking into account that at equilibrium a† b = b† a, the comparison with eqn (15.61) then yields Φ0 = 0 and the identiﬁcation V =

1 † a b + b† a N

(15.95)

Boson Hubbard Hamiltonian

301

for the visibility factor. Notice that with this formalism we do not need to deﬁne the phase operator in order to calculate the visibility of interference fringes. A simple calculation gives

δN0 1 δJ + N EC /4 V =1−2 =1− −1 . (15.96) N N εJ # C In the Josephson regime N EC δJ one gets V ≈ 1− 14 E EJ , in agreement with (15.60) and (15.65). Also, in the opposite limit EC → 0 (absence of interactions) one ﬁnds that V → 1.

Part III

16 Interacting Fermi Gases and the BCS–BEC Crossover The following Chapters (from 16 to 20) are devoted to the study of interacting Fermi gases. As anticipated in the Introduction, these systems have become the object of intense experimental and theoretical research in recent years. After a brief summary of the properties of the ideal Fermi gas (Section 16.1), the present chapter focuses on the properties of dilute interacting Fermi gases. The weakly repulsive Fermi gas is discussed in Section 16.3, while in Sections 16.4 and 16.5 we discuss, respectively, the gas of composite bosons and the BCS limit of a weakly interacting Fermi gas. The main properties of the strongly interacting (but still dilute) unitary Fermi gas, where the scattering length is much larger than the average interatomic distance, are discussed in Section 16.6. Some general features of the BCS–BEC crossover are discussed in Section 16.7, while in Section 16.8 we derive the formalism of the mean-ﬁeld Bogoliubov–de Gennes approach. A discussion of the main physical quantities predicted by mean-ﬁeld theory and by Quantum Monte Carlo simulations, including, in particular, the equation of state, the momentum distribution, and the condensation of pairs, is presented in Section 16.9.

16.1

The ideal Fermi gas

In this section we recall some basic features of the ideal Fermi gas model. This model provides a benchmark of fundamental relevance in diﬀerent domains of physics. Due to the Pauli principle, no quantum state can be occupied by more than one fermion with the same quantum numbers, and the many-body eigenstates of the Hamiltonian are described in terms of Slater determinants, ensuring the proper antisymmetry property of the wave function. This is a major diﬀerence to the case of bosons, and for this reason the ideal Fermi gas can not exhibit the phenomenon of Bose–Einstein condensation. Interactions can, however, change the many-body scenario in a signiﬁcant way, giving rise to pairing phenomena, condensation of pairs, and superﬂuid eﬀects, as we will extensively discuss in the following sections. We will consider fermions occupying either one or two internal spin states, hereafter called, for simplicity, spin up (σ = ↑) and spin down (σ = ↓). The ideal Fermi gas is characterized by the well-known law n ¯ σ,i =

1 eβ(i −μσ ) + 1

(16.1)

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

306

Interacting Fermi Gases and the BCS–BEC Crossover

for the average occupation numbers of the ith single-particle state with spin σ. This law can easily be derived in the framework of the grand canonical ensemble. Here μσ is the chemical potential ﬁxed by the normalization condition n ¯ σ,i . (16.2) Nσ = i

Since spontaneous transitions between the spin states are inhibited one can assume that N↑ and N↓ are conserved quantities and hence in general μ↑ = μ↓ . With respect to the corresponding result (3.14), which holds for the ideal Bose gas, the sign + in the denominator in (16.1) reﬂects the consequence of the condition of antisymmetry imposed on the many-body wave function by the Pauli exclusion principle. At T = 0, where the chemical potential μσ of the ideal Fermi gas deﬁnes the value of the Fermi temperature EF,σ , one ﬁnds n ¯ σ,i = 1 for i < EF,σ and n ¯ σ,i = 0 for i > EF,σ . In a uniform√ system occupying a volume V , the single-particle states are plane waves ϕp = (1/ V )eip·r/ and p = p2 /2m with the momentum p ﬁxed by the usual periodic boundary conditions p = 2πn/L where n is a vector whose components nx , ny , nz are 0 or ± integers. The total number of particles occupying each spin state is then given, in the thermodynamic limit, by V g() Nσ = , (16.3) dk n ¯ = d β(−μ ) σ,k σ + 1 (2π)3 e where g is the density of single-particle states of uniform matter (see eqn (10.14)), while the Fermi energy takes the simple value EF,σ = kB TF,σ =

2 (6π 2 nσ )2/3 , 2m

(16.4)

ﬁxed by the density nσ = Nσ /V . One can also write EF,σ = (2 /2m)p2F,σ where pF,σ = (6π 2 nσ )1/3 is the Fermi momentum. Equation (16.4) ﬁxes an important energy (and temperature) scale in the problem that will also used in the case of interacting systems. At ﬁnite temperatures all the thermodynamic functions of the ideal threedimensional uniform Fermi gas can be expressed in terms of the integrals ∞ ∞ 1 1 (−1)+1 z Fp (z) = = dxxp−1 −1 x , (16.5) Γ(p) 0 z e +1 p =1

where z = exp(βμσ ), which are the fermionic counterpart of the bosonic integrals gp (z) introduced in eqn (3.26). For example, the density and the pressure can be written as nσ λ3T = F3/2 (z)

(16.6)

Pσ βλ3T = F5/2 (z),

(16.7)

and respectively, where λT = 2π2 /mkB T is the thermal wavelength.

The weakly repulsive Fermi gas

16.2

307

Dilute interacting Fermi gases

The ideal gas model described in the previous section provides a good description of a cold spin-polarized Fermi gas (N↑ = N , N↓ = 0). In this case the eﬀects of short-range interactions are in fact inhibited by the Pauli exclusion principle. When atoms occupy diﬀerent spin states, interactions can instead strongly aﬀect the solution of the manybody problem. This is particularly true at very low temperatures, where an attractive force can give rise to pairing eﬀects responsible for a superﬂuid behaviour. Dilute gases are characterized by the condition r0 d, where r0 is the typical range of the two-body force and d ∼ n−1/3 , with n the total density, is the average interparticle distance. In these systems the s-wave scattering length, characterizing the low-energy scattering between two fermions occupying diﬀerent spin states, turns out to be the crucial interaction parameter for classifying the physical properties of the many-body system at low temperatures, where the scattering lengths with higher angular momentum provide minor contributions. It is worth mentioning that in a dilute Fermi gas the conditions of stability do not impose restrictions on the value of the scattering length; in particular, the scattering length can be either positive or negative. Furthermore, its value can be smaller or larger than the interparticle average separation. This is a major diﬀerence with respect to the case of Bose gases, where the scattering length should be positive to ensure the stability of uniform conﬁgurations, and the stability conditions against losses and three-body recombinations require that the gas should be weakly interacting (na3 1; see Chapter 4). The many-body solution of the interacting Fermi gas is actually also well deﬁned for a < 0, as a consequence of the stabilizing eﬀect of the Fermi pressure. In the |a| d limit this solution corresponds to the celebrated BCS regime typical of superconductivity. In the Fermi case, thanks to the consequences of the Pauli exclusion principle, one can also reach long-lived conﬁgurations for large values of the scattering length. In other words, the gas can simultaneously be dilute (r0 d) and strongly interacting, in the sense that the scattering length can be larger than the interatomic distances. In this context the most interesting case is the so-called unitary Fermi gas characterized by the condition a d (see Section 16.6). The availability of broad Fano–Feshbach resonances in Fermi gases, allowing for a controlled tuning of the scattering length via an external magnetic ﬁeld (see Chapter 9), has initiated in recent years a wonderful way to study the interaction and superﬂuid eﬀects in atomic Fermi gases. In particular, it has been possible to investigate systematically the crossover from the BCS regime of small and negative scattering lengths to the regime of small and positive scattering lengths, where bound dimers of atoms with diﬀerent spin are formed, giving rise to Bose–Einstein condensation of dimers. In the following we will discuss some of the most relevant features of these interesting conﬁgurations.

16.3

The weakly repulsive Fermi gas

There are important cases in which the many-body problem for the interacting Fermi gas can be solved in an exact way. A ﬁrst example is the dilute repulsive branch. Let us consider a dilute uniform Fermi gas with equal numbers of particles in the two spin

308

Interacting Fermi Gases and the BCS–BEC Crossover

states (n↑ = n↓ = n/2) and interacting with a positive value of the scattering length satisfying the condition na3 1 or, equivalently, akF 1 where kF = (3π 2 n)1/3 is the Fermi momentum. Applying perturbation theory with the pseudo potential (9.22), starting from the ground state of the ideal Fermi gas, one ﬁnds the expansion (Huang and Yang, 1957; Lee and Yang, 1957)

Epert 3 10 4(11 − 2 ln 2) 2 = EF 1 + kF a + (kF a) + . . . (16.8) N 5 9π 21π 2 for the energy, where E F = kB T F =

2 (3π 2 n)2/3 2m

(16.9)

is the Fermi energy of the unpolarized Fermi gas and TF the corresponding temperature. The expansion (16.8) holds for small values of the dimensionless parameter kF a and has universal character up to the term in a2 . Higher-order corrections in the scattering length will instead depend on the details of the potential. In the case of purely repulsive potentials, such as the hard-sphere model, the expansion (16.8) corresponds to the ground state energy of the system (Lieb et al., 2005; Seiringer, 2006). For more realistic potentials, with an attractive tail, the above result describes the metastable branch of the repulsive atomic gas. This speciﬁcation is particularly important in the presence of bound states at the two-body level, since lower-energy conﬁgurations, satisfying the same condition kF a 1, consist of a gas of dimers (see next section). The weakly repulsive gas remains normal down to extremely low temperatures when the repulsive potential produces > 0 pairing eﬀects, bringing the system into a superﬂuid phase (Kohn and Luttinger, 1965). Another important property characterizing the repulsive Fermi gas is the momentum distribution n(p), related to the occupation number nk of the single-particle states by the relation n(p) = V /(2π)3 nk with p = k. The function nk diﬀers from the Θ(k − kF ) behaviour of the ideal Fermi gas model. The problem was solved by Belyakov (1961) using perturbation theory up to second-order terms in the scattering length (see also Migdal, 1957; Galitskii, 1958). In particular, the jump at the Fermi surface is given by nk− − nk+ = 1 − F

F

4 ln 2(kF a)2 , π2

(16.10)

while at large k interactions are responsible for a typical 1/k4 behaviour according to the law 2 4 kF 2kF a nk → . (16.11) 3π k Of course result (16.11) holds under the condition that k is smaller than the inverse of the range of the potential. The atomic repulsive gas conﬁguration has been experimentally achieved in a Fermi gas by ramping up adiabatically the value of the scattering length (Bourdel et al., 2003;

Gas of composite bosons

309

Jo et al., 2009), starting from the value a = 0 where the many-body state corresponds to the ideal Fermi gas. If one stays suﬃciently far from the resonance, losses caused by the transition to the more stable molecular conﬁguration (see next section) are not important and the lifetime of the conﬁguration is long enough. The magnetic properties of the repulsive Fermi gas will be discussed in Section 20.1.

16.4

Gas of composite bosons

In Chapter 9 we showed that, due to the availability of Feshbach resonances, it is possible to tune the value of the scattering length in a highly controlled way. For example, starting from a negative and small value of the scattering length one can increase the value of a, reach the resonance, and explore the other side of the resonance where a becomes positive and eventually small. One might naively expect in this case to reach the regime of the weakly repulsive gas discussed in the previous section. This is not the case because, in the presence of a Feshbach resonance, the positive value of the scattering length is associated with the emergence of a weakly bound state in the two-body problem and the consequent formation of dimers (also called Feshbach molecules) with wave function 1 −r/a e . (16.12) r The size of these dimers is ﬁxed by the scattering length a and their binding energy is b = −2 /ma2 . They have a bosonic nature, being composed of two fermions, and if the gas is suﬃciently dilute and cold they give rise to Bose–Einstein condensation. The size of the dimers cannot, however, be too small, as it should remain large compared to the size of the deeply bound energy levels of the molecules whose size is ﬁxed by the typical range of the potential. This condition ensures, in particular, that dimers are stable against the transition to deeper molecular states due to collisions. Unlike the repulsive gas of atoms discussed in the previous section, the gas of dimers cannot be described using perturbation theory starting from the ideal Fermi gas ground state. It instead requires a non-perturbative approach. The two pictures (repulsive gas and gas of dimers) actually represent two diﬀerent branches of the many-body problem, both corresponding to positive and small values of the scattering length. The gas of dimers, which is the lower and hence energetically more stable branch, can in practice be realized by crossing adiabatically the Feshbach resonance starting from negative values of a, which allows for an eﬃcient conversion of pairs of atoms into molecules, or by cooling down a gas with a ﬁxed (positive) value of the scattering length. The behaviour of the dilute (kF a 1) gas of dimers, hereafter called the BEC limit, is described by the theory of Bose–Einstein condensation discussed here in previous chapters. One can easily evaluate the critical temperature for the occurrence of Bose– Einstein condensation in the ideal uniform gas (see eqn (3.28)) and express it in terms of the Fermi temperature (16.4). One ﬁnds φ(r) =

Tc = 0.218TF , where TF is the Fermi temperature (16.9) and n = 2nσ is the total density.

(16.13)

310

Interacting Fermi Gases and the BCS–BEC Crossover

The occurrence of Bose–Einstein condensation of dimers emerging from an interacting Fermi gas has been experimentally proven (Greiner et al., 2003; Zwierlein et al., 2003; Bourdel et al., 2004; Bartenstein et al., 2004a; Partridge et al., 2005) by measuring the typical bi-modal distribution of the density proﬁle after expansion, which is the characteristic feature of Bose–Einstein condensation in harmonically trapped conﬁgurations (see Figure 1.2). Interactions among dimers yield the Bogoliubov gas widely discussed in the previous chapters of this volume. One should recall that in the case of composite bosons emerging from a gas of interacting fermions the mass of constituents is equal to twice the mass of single atoms and that the dimer–dimer scattering length should not be confused with the atomic scattering length characterizing the interaction between fermions. The identiﬁcation of the dimer–dimer scattering length, which is the key parameter needed to calculate the equilibrium as well as the dynamic behaviour of the interacting BEC gas of dimers, represents a nontrivial scattering problem. Using the zero-range approximation together with the contact boundary condition (9.18) Petrov et al. (2004) solved exactly the problem, obtaining the important result add = 0.60a,

(16.14)

which provides a nontrivial link between the dimer–dimer scattering length and the atomic scattering length. The same approach provides the result aad = 1.18a for the atom–dimer scattering length (Petrov, 2003). The problem of the scattering between atoms and weakly bound dimers was actually ﬁrst investigated by Skorniakov and Ter-Martirosian (1956) in connection with neutron–deuteron scattering. It is worth pointing out that, by applying the Born approximation, one would instead ﬁnd the results add = 2a and aad = 8a/3 (Pieri and Strinati, 2006). Starting from the knowledge of add one can calculate the beyond-mean-ﬁeld corrections to the equation of state of the interacting Fermi gas in the BEC regime by replacing m with 2m and a with add in the bosonic coupling constant entering the expansion (4.33) which then takes the form # N 128 π2 add E = b + N nd 1 + √ nd a3dd + . . . , (16.15) 2 2m 15 π where N is the total number of atoms, nd is the dimer density, and, with respect to eqn (4.33), we have also added the binding energy term b of a noninteracting dimer. The equation of state of the weakly interacting gas of dimers was measured by Navon et al. (2010) exploring the BEC side of the resonance of an ultracold interacting Fermi gas, conﬁrming at the same time the validity of result (16.14) for the dimer–dimer interaction and of the Lee–Huang–Yang correction of eqn (16.15). The weakly bound dimers formed near a Feshbach resonance are molecules in the highest roto-vibrational bound state. Due to collisions they can fall into deeper bound states of size of the order of the interaction range r0 . In this process a large energy of order 2 /mr02 is released and converted into kinetic energy of the colliding atoms, causing atomic losses. In the case of atom–dimer collisions one can estimate the probability of the three atoms approaching each other within distances ∼ r0 . This probability is suppressed by the Pauli principle, because two of the three atoms have

The BCS limit of a weakly attractive gas

311

αdd [10–13 cm3·S–1]

10

1

0.1 40

100 a [nm]

200

Figure 16.1 The dimer recombination coeﬃcient αdd as a function of the scattering length a. The slope of the dashed line corresponds to the theoretical dependence αdd ∝ a−2.5 . From c 2005, IOP Petrov et al. (2005). Reprinted by permission Journal Physics B, 38, 5645; Publishing.

the same spin. A description of the relaxation process is provided by the equation n˙ a = −αad na nd , where na and nd are, respectively, the densities of atoms and of dimers, and n˙ a is the rate of atom losses. For the atom–dimer relaxation coeﬃcient αad the following dependence on a has been predicted (Petrov et al., 2004): αad ∝

r0 r0 s , m a

(16.16)

with s = 3.33. In the case of relaxation processes caused by dimer–dimer collisions, the coeﬃcient entering the dimer loss equation n˙ d = −αdd n2d satisﬁes the same law (16.16) with s = 2.55. It is crucial that both αad and αdd decrease with increasing a. This dependence ensures the stability of Fermi gases near a Feshbach resonance. It is the consequence of the fermionic nature of the atoms. In the case of bosons, instead, the relaxation time increases with increasing a and the system becomes unstable approaching the resonance. According to the above results, the dimer–dimer relaxation rate should dominate over the atom–dimer rate in the limit r0 /a → 0. Experiments on atomic losses both in potassium (Regal et al., 2004a) and in lithium (Bourdel et al., 2004; Petrov et al., 2005) close to the Feshbach resonance give relaxation rate constants αdd ∝ a−s with values of the exponent s in reasonable agreement with theory (see Figure 16.1).

16.5

The BCS limit of a weakly attractive gas

When the scattering length is small and negative the interacting Fermi gas exhibits very diﬀerent features as to those of positive scattering lengths discussed in the

312

Interacting Fermi Gases and the BCS–BEC Crossover

two previous sections. At low enough temperatures the Fermi gas is, in fact, unstable against the formation of bound states—the Cooper pairs—which have an exponentially small binding energy (Cooper, 1956). The resulting many-body conﬁguration corresponds to the most famous BCS picture ﬁrst introduced to describe the phenomenon of superconductivity (Bardeen, Cooper, and Schrieﬀer, 1957). The many-body solution proceeds through a proper diagonalization of the Hamiltonian, which is obtained by applying the Bogoliubov transformations to the Fermi ﬁeld operators (Bogoliubov, 1958a,b) as we will discuss in Section 16.8. This approach is non-perturbative and predicts a second-order phase transition. It is worth mentioning that the Cooper pairs diﬀer from the dimers discussed in the previous section in a signiﬁcant way: while the dimers correspond to the bound state of the two-body problem and exist only for positive and small values of kF a, Cooper pairs are instead embedded in the many-body conﬁguration. Their existence is predicted for negative values of a and their size is much larger than the average interparticle distance. We refer to the resulting many-body conﬁguration for negative values of a, satisfying the condition kF |a| 1, as the BCS limit. The transition from the BCS regime of Cooper pairs to the BEC regime of condensed dimers through the Feshbach resonance represents a challenging many-body problem that will be discussed in Sections 16.7 and 16.8. In the BCS regime an exact result is available for the critical temperature, resulting in the expression (Gorkov and Melik-Barkhudarov, 1961) 7/3 γ 2 Tc = TF e−π/2kF |a| ≈ 0.28TF e−π/2kF |a| , (16.17) e π where γ = eC 1.781, C being the Euler constant. The exponential, non-analytical dependence of Tc on the interaction strength kF |a| is typical of the BCS regime. With respect to the original treatment by Bardeen, Cooper, and Schrieﬀer (1957), the preexponential term in eqn (16.17) is a factor ∼2 smaller as it accounts for the renormalization of the scattering length due to screening eﬀects in the medium (Pethick and Smith, 2008). In the BCS regime one can also calculate the spectrum of single-particle excitations close to the Fermi surface, |k − kF | kF : # k = Δ2gap + [vF (k − kF )]2 , (16.18) where vF = kF /m is the Fermi velocity, and it is minimum at k = kF . The gap at T = 0 is related to the critical temperature Tc through the expression π (16.19) Δgap = kB Tc ≈ 1.76kB Tc . γ Furthermore, the ground-state energy per particle takes the form 3Δ2gap Epert E = − , N N 8EF

(16.20)

where Epert is the perturbation expansion (16.8) with a < 0, and the term proportional to Δ2gap corresponds to the exponentially small energy gain of the superﬂuid compared

Gas at unitarity

313

to the normal state. The gap also provides the estimate vF /Δgap for the size of the Cooper pairs, which turns out to be increasingly large as one approaches the kF |a| → 0 limit. Since the transition temperature Tc becomes exponentially small as one decreases the value of kF |a|, the observability of superﬂuid phenomena in the BCS regime is a diﬃcult task in dilute gases. Furthermore, in the experimentally relevant case of harmonically trapped conﬁgurations the predicted value for the critical temperature easily becomes smaller than the oscillator temperature ωho /kB , and the superﬂuid phenomena cannot simply be described in terms of many-body theories based on uniform conﬁgurations, but should include ﬁnite size and shell eﬀects, as happens in nuclear physics (see, for example, Bohr and Mottelson, 1969; Ring and Schuck 1980). First approaches of BCS theory to ultracold atomic Fermi gases were provided by Stoof et al. (1996) and Houbiers et al. (1997).

16.6

Gas at unitarity

A more diﬃcult problem, compared to the BCS and BEC regimes discussed in the previous sections, concerns the behaviour of the many-body system when kF |a| is of the order or even larger than 1, i.e. when the scattering length is of the order or larger than the interparticle distance, which, in turn, is much larger than the range of the interatomic potential. This corresponds to the unusual situation of a gas which is dilute and strongly interacting at the same time. In this condition, it is not easy to predict whether the system is stable or will collapse. Moreover, if the gas remains stable, does it exhibit superﬂuidity as in the BCS and BEC regimes? Since at present an exact solution of the many-body problem for kF |a| > 1 is not available, one has to resort to approximate schemes or numerical simulations. These approaches, together with the experimental results, give a clear indication that the gas is indeed stable and that it is superﬂuid below a critical temperature. The limit kF |a| → ∞ is called the unitary regime, already introduced in Section 9.2 in the discussion of two-body collisions. This regime is characterized by the universal behaviour of the scattering amplitude f0 (k) = i/k, which bears important consequences at the many-body level. As the scattering length drops out of the problem, the only relevant length scales remain the inverse of the Fermi wave vector and the thermal wavelength. All thermodynamic quantities should therefore be universal functions of the Fermi energy (16.9) ﬁxed by the density, and of the ratio T /TF . An important example of this universal behaviour is provided by the T = 0 value of the chemical potential. Due to the dimensional considerations discussed above the chemical potential should be proportional to the Fermi energy μ = ξB EF ,

(16.21)

the coeﬃcient of proportionality ξB , being a dimensionless number, called the Bertsch parameter (Bertsch, 1999; see also Heiselberg, 2001). This relation ﬁxes the density dependence of the equation of state, with nontrivial consequences on the density proﬁles and on the collective frequencies of harmonically trapped superﬂuids, as we will discuss in Chapters 18 and 19. The value of ξB has been calculated using quantum

314

Interacting Fermi Gases and the BCS–BEC Crossover

Monte Carlo techniques (Carlson et al., 2003; Astrakharchik et al., 2004a). The most recent estimate by Carlson et al. (2011) provides the value 0.37, in excellent agreement with the experimental determination by Ku et al. (2012). The fact that the value of ξB is smaller than 1 reﬂects the attractive nature of interactions at unitarity. By integrating eqn (16.21) one ﬁnds that the coeﬃcient ξB also relates the ground state energy per particle E/N and the pressure P to the corresponding ideal gas values: E/N = ξB 3EF /5 and P = ξB 2nEF /5, respectively. According to the usual thermodynamic relation mc2 = n∂μ/∂n, the speed of sound is given by the expression 1/2 vF c = ξB √ , 3

(16.22)

Tc = αTF ,

(16.23)

√ where vF / 3 is the speed of sound for an ideal Fermi gas. The superﬂuid gap at T = 0 should also scale with the Fermi energy and numerical calculations yield the value Δgap = (0.50 ± 0.03)EF (Carlson et al., 2003; Carlson and Reddy, 2005). At ﬁnite temperatures the most relevant problem, both theoretically and experimentally, is the determination of the transition temperature Tc which, again for dimensionality arguments, is expected to be proportional to the Fermi temperature:

where α is a dimensionless universal parameter. The most recent reliable theoretical calculations, based on quantum Monte Carlo (Burovski et al., 2006a,b; Goulko and Wingate, 2010) and diagrammatic (Haussmann et al., 2007) techniques, are in good agreement with the experimental value α = 0.167 determined by Ku et al. (2012). Since at unitarity the gas is strongly correlated, one expects a signiﬁcantly large critical region near Tc . Furthermore, the phase transition should belong to the same universality class, corresponding to a complex order parameter, as the one in bosonic ﬂuids and should exhibit similar features including the characteristic λ singularity of the speciﬁc heat. At ﬁnite temperatures an additional length scale is the thermal wavelength (3.24) and the energy scales are now the temperature and the Fermi temperature (16.4) or, alternatively, the chemical potential μ. It follows that at unitarity all the thermodynamic functions can be expressed (Ho, 2004) in terms of a universal function fp (x) depending on the dimensionless parameter x ≡ βμ where β = 1/kB T . This function can be deﬁned in terms of the pressure of the gas, according to the relationship P βλ3T = fp (x),

(16.24)

nλ3T = fp (x) ≡ fn (x).

(16.25)

2π2 /mkB T is the thermal wavelength. Using the thermodynamic where λT = relation n = (∂P/∂μ)T , the density of the gas can then be written as

From eqn (16.25) one also derives the useful relationship T 4π = TF [3π 2 fn (x)]2/3

(16.26)

Gas at unitarity

315

for the ratio between the temperature and the Fermi temperature in terms of the ratio x between the chemical potential and the temperature of the gas. In terms of fn and fp we can calculate all the thermodynamic functions of the unitary Fermi gas. For example, using the thermodynamic relation S/N = −(∂μ/∂T )P , we ﬁnd the result S s 5 fp = = − x, N kB nkB 2 fn

(16.27)

for the entropy, while the speciﬁc heats at constant volume and pressure become CV 15 fp 9 fn = − , N kB 4 fn 4 fn and CP = N kB

9 fn 15 fp − 4 fn 4 fn

5 fn fp . 3 fn2

In similar way one can derive the results 1 ∂n βλ3T fn = κT = n ∂P T,N fn2 and 1 κs = n

∂n ∂P

= S,N

3 βλ3T 5 fp

(16.28)

(16.29)

(16.30)

(16.31)

for the isothermal and adiabatic compressibilities, whose ratio coincides with the ratio between CP and CV . It is worth noting that the above equations for the thermodynamic functions of the unitary Fermi gas are formally identical to the ones of the ideal Fermi gas, the dimensionless functions fp and fn replacing, apart from a factor 2 caused by spin degeneracy, the F5/2 and F3/2 Fermi integrals of Section 16.1. The above equations are consistent with the general rules of thermodynamics, according to which the speciﬁc heat at constant volume cannot diverge at the critical point. According to eqn (16.28) an upper bound to CV is obtained by setting fn = ∞, corresponding to a divergent value of the speciﬁc heat at constant pressure. This provides the rigorous inequality CV /N kB ≤ (15/4)fp /fn = (15/4)P/(nkB T ). Equation (16.27) shows that the entropy only depends on the dimensionless parameter x, or, according to eqn (16.26), on the ratio T /TF . From eqns (16.24) and (16.25) one then ﬁnds that during an adiabatic transformation the quantity P/n5/3 remains constant, which is the same condition characterizing a noninteracting monoatomic gas. The scaling function fp (x) (and hence its derivative fn (x)) can be determined through microscopic many-body calculations, or extracted directly from experiments carried out in trapped conﬁgurations, from which it is possible to build the equation of state of uniform matter, following the procedure discussed in Section 13.6. In Figure 16.2 we show the most relevant result for the equation of state βμ as a

316

Interacting Fermi Gases and the BCS–BEC Crossover 6 8

6

μ / kBT

μ /kBT

4

4

2

2

0 0.05

0.10

0

–2 0.0

TC / TF 0.5

1.0

0.15 TC / TF 0.20 T/TF

0.25

1.5

2.0

T/TF

Figure 16.2 Equation of state μ/kB T versus T /TF . The dash-dotted line corresponds to the phonon contribution to thermodynamics. The ﬁlled circles correspond to the experiment data by Ku et al. (2012) in the higher T regime, while the solid line corresponds to the virial expansion in classical limit. The arrows indicate the critical point Tc /TF = 0.167(13). The inset is an ampliﬁcation in the lower T regime. From Hou et al. (2013b).

function of T /TF . The theoretical behaviour of the scaling functions is determined by exact thermodynamic relations for x → +∞ (low temperature, phonon regime) and for x → −∞ (high temperature). In the former case one ﬁnds

3/2 5/2 2 (4π)3/2 π4 3 x fp (x → +∞) = ξB + + ... , 5 3π 2 ξB 96 x

(16.32)

where ξB is the Bertsch parameter. The ﬁrst term in the expansion determines the T = 0 value of the thermodynamic functions, while the second one accounts for the ﬁrst contribution due to the thermal excitation of phonons. In the latter case one instead ﬁnds fp (x → −∞) = 2 ex + b2 e2x + b3 e3x + . . . ,

(16.33)

where the ﬁrst term is the classical result, the factor 2 arising from spin degeneracy, while the coeﬃcients b2 and b3 are related to the second and third virial coeﬃcients (see following discussion). The behaviour in the most relevant region around TC , corresponding to x ∼ 1, is much more uncertain from the theoretical point of view. In the intermediate region we

Gas at unitarity

317

1.6

0.8 0.4 0.0 4

4

C/NkB

3 2

2

C/NkB

S/NkB

1.2

1 0 0.0

0 0.00

0.2

0.4 0.6 T/TF

0.04

0.8

0.08

1.0

0.12

0.16

0.20

0.24

T/TF Figure 16.3 Entropy and speciﬁc heats per particle in uniform matter, evaluated using eqns (16.27)–(16.29) and the experimental data by Ku et al. (2012). In the lower panel, the square-guided line corresponds to Cp /N kB ; the circle-guided line to Cv /N kB ; the inset is for the speciﬁc heats in a large temperature interval. The vertical line indicates the critical temperature. From Hou et al. (2013b).

report the values determined directly from experiments (Ku et al., 2012), with proper matching procedures at low and high temperatures (Hou et al. 2013b). In Figure 16.3 we show the relevant thermodynamic functions S/N kB , CV /N kB , and CP /N kB as functions of T /TF . One can see that the characteristic λ-like behaviour is clearly exhibited by the speciﬁc heats, allowing for the experimental determination of the critical value xc = 2.48 corresponding to the result TC = 0.167TF (Ku et al., 2012) for the critical temperature ﬁxing the transition between the superﬂuid and the normal phase. Previous experimental measurements of the equation of state of the unitary Fermi gas were reported by Horikoshi et al. (2010) and Nascimbene et al. (2010b). As already mentioned (see eqn (16.33)) the scaling equations also hold at high temperatures, T TF . This is, however, only ensured if the thermal √ wavelength is still large compared to the eﬀective range of the interaction, / mkB T r0 . In this regime of temperatures the unitary gas can be described, to ﬁrst approximation, by an ideal Maxwell–Boltzmann gas. First corrections to the equation of state are usually expressed in terms the second virial coeﬃcient B(T ) deﬁned from the

318

Interacting Fermi Gases and the BCS–BEC Crossover

expansion of the pressure P nkB T [1 + nB(T )]. Using the method of partial waves (Beth and Uhlenbeck, 1937; Landau and Lifshitz, 1980) and accounting for the unitary contribution of the s-wave phase shift δ0 = ∓π/2 when a → ±∞, one obtains the result

B(T ) =

−λ3T

b2 3 =− 2 4

π2 mkB T

3/2 ,

(16.34)

√ corresponding to b2 = 3/ 32. It is worth noting that the negative sign of the second virial coeﬃcient corresponds to attraction. Equation (16.34) takes into account both the eﬀects of Fermi statistics and interaction. The pure statistical contribution would be given by the same expression in brackets, but with the coeﬃcient +1/4 of opposite sign. Results for the third virial coeﬃcient of the unitary Fermi gas have also recently been calculated by Liu et al. (2009) who found the value b3 = −0.29. The theoretical predictions for the second and third virial coeﬃcients have been experimentally conﬁrmed with good accuracy (Nascimbene et al., 2010b; Ku et al., 2012). Let us ﬁnally point out that, except at very low temperatures, the superﬂuid density ns cannot be expressed in terms of the thermodynamic functions and cannot

1.2 1.0

ns/n

0.8 0.6 0.4 0.2 0.0 0.0

0.2

0.4

0.6 T/Tc

0.8

1.0

Figure 16.4 Superﬂuid fraction for uniform resonantly interacting Fermi gas versus T /Tc . The points represent the experimental data of Sidorenkov et al. (2013), the shaded region being the corresponding uncertainty range. The two horizontal error bars indicate the systematic uncertainties resulting from the limited knowledge of the critical temperature Tc . The fraction for helium II (solid line) as measured in Dash and Taylor (1957) and the textbook expression 1 − (T /Tc )3/2 for the Bose–Einstein condensed fraction of the ideal Bose gas (dashed line) are shown for comparison.

The BCS–BEC crossover

319

consequently be parameterized in terms of the scaling functions introduced above. At unitarity, according to dimensional arguments it can be written as ns (T, x) =

1 fs (x), λ3T

(16.35)

where fs is another scaling function of the dimensionless variable x. In addition to the low-temperature phonon regime (see eqn (6.11)), the behaviour of ns is known near the critical point, where it is expected to vanish according to the law (Josephson, 1966) ns ∝ (1 − T /TC )2/3 .

(16.36)

First experimental results for the superﬂuid density in the unitary Fermi gases have recently become available (Sidorenkov et al., 2013) from the measurement of the speed of second sound (see Section 19.5). The extracted experimental values are shown in Figure 16.4 and compared with the experimental values measured in superﬂuid 4 He. When expressed in terms of T /TC the two curves look similar.

16.7

The BCS–BEC crossover

In the previous sections we described general features of interacting Fermi gases in relevant asymptotic limits where the many-body description can be formulated and solved in an exact way. These include the case of a dilute gas of dimers, corresponding to positive (and small) values of the scattering length, and the BCS regime of Cooper pairs, corresponding to negative (and small) values of the scattering length. The description of the transition between these two diﬀerent regimes has attracted the attention of a large community of scientists in recent years. The general scenario emerging from these studies, initially started in the context of superconductivity, is summarized in Figure 16.5, where above Tc , on the BCS side, one identiﬁes a normal Fermi liquid where Cooper pairs are dissociated. On the BEC side pairs are instead still tightly bound above Tc , although they are not Bose–Einstein condensed. The two regions above Tc are separated by the pair-formation crossover scale T ∗ (for recent experimental and theoretical investigations of the pseudo-gap behaviour, see Gaebler et al. (2010) and the review book edited by Zwerger (2012)). The value of the critical temperature as a function of 1/kF a in the ﬁgure corresponds to the prediction of BCS mean-ﬁeld theory (S´ a de Melo et al., 1993). The asymptotic limits of the critical temperature in the BEC and BCS regimes are well understood (see eqns (16.13) and (16.17)), while the most reliable theoretical estimate at unitarity, shown as a diamond in the ﬁgure and now also conﬁrmed experimentally, is Tc = 0.167TF (see previous section). The possibility of exploring the resonance region, where the scattering length can take values much larger than the average interparticle distance (the so-called unitary limit, see previous section), is particularly challenging because of the emergence of strong interaction eﬀects and unique universal features. Tremendous progress in the understanding of the transition has recently been achieved from both experimental and theoretical points of view. There is now general consensus that the transition between the BCS regime of small and negative values of a and the BEC

320

Interacting Fermi Gases and the BCS–BEC Crossover 0.6 unbound fermions

pairing

T*

0.4

T/EF

normal Bose liquid Tc

pseudogap condensation

0.2

normal Fermi liquid

superfluid unitarity

0 –2 BCS

–1

1/(kFas)

0

1 BEC

Attraction

Figure 16.5 Transition temperature in units of the Fermi energy EF as a function of the interaction strength along the BCS–BEC crossover, calculated using BCS mean-ﬁeld theory. From Randeria (2010). The pair-formation crossover temperature T ∗ is also shown (see text). The diamond corresponds to the theoretical prediction for TC by Burovski et al. (2006a) based on a quantum Monte Carlo simulation at unitarity.

regime of small and positive values of a is characterized by a continuous crossover (the so-called BCS–BEC crossover) through the unitary point, without any discontinuity in the thermodynamic functions. At ﬁrst sight this is a surprise because the BCS regime of superconductivity, characterized by the emergence of Cooper pairs, and the gas of dimers exhibit very diﬀerent features. All these regimes actually share, in three dimensions and at low temperatures, a common crucial feature which is at the origin of their superﬂuid behaviour: the existence of oﬀ-diagonal long-range order (ODLRO), according to the asymptotic behaviour (Gorkov, 1958) ˆ † (r2 + r)Ψ ˆ † (r1 + r)Ψ ˆ ↓ (r1 )Ψ ˆ ↑ (r2 ) = |F (r1 , r2 )|2 lim Ψ ↑ ↓

r→∞

(16.37)

The BCS–BEC crossover

321

exhibited by the two-body density matrix. For this reason the repulsive gas of fermions discussed in Section 16.3 is not playing any role in the discussion of the present section, since it belongs to a diﬀerent branch in the phase diagram, corresponding to the normal (non-superﬂuid) phase of the interacting Fermi gas. By assuming spontaneous breaking of gauge symmetry one can introduce the pairing ﬁeld ˆ ↓ (R + s/2)Ψ ˆ ↑ (R − s/2). F (R, s) = Ψ

(16.38)

The vectors R = (r1 +r2 )/2 and s = r1 −r2 denote, respectively, the centre of mass and the relative coordinate of the pair of particles. In a Fermi superﬂuid ODLRO involves the expectation value of the product of two ﬁeld operators instead of a single ﬁeld operator as in the case of Bose–Einstein condensation (see Chapter 2). The pairing ﬁeld in eqn (16.38) refers to spin-singlet pairing and the spatial function F must satisfy the even-parity symmetry requirement F (R, −s) = F (R, s), imposed by the anticommutation rule of the ﬁeld operators. The use of the Bethe–Peierls boundary conditions (9.18) for the many-body wave function Ψ implies that the pairing ﬁeld (16.38) is proportional to (1/s − 1/a) for small values of the relative coordinate s. One can then write the following short-range expansion: m 1 1 F (R, s) = − + o(s), (16.39) Δ(R) 4π2 s a which deﬁnes the quantity Δ(R), hereafter called the order parameter. For uniform systems the dependence on the centre-of-mass coordinate R in eqns (16.38) and (16.39) drops out and the order parameter Δ becomes constant. Moreover, in the case of s-wave pairing, the function (16.38) becomes spherically symmetric: F = F (s). The pairing ﬁeld F (s) can be interpreted as the wave function of the macroscopically occupied two-particle state. The condensate fraction of pairs is then deﬁned according to 1 ncond = ds |F (s)|2 , (16.40) n/2 where ds|F (s)|2 is the density of condensed pairs. The quantity ncond is exponentially small for large, weakly bound Cooper pairs. It instead approaches the value ncond 1 for small, tightly bound dimers that are almost fully Bose–Einstein condensed at T = 0. The order parameter characterizes in a fundamental way the superﬂuid phase and its vanishing ﬁxes the transition to the normal phase at the critical temperature TC . It is a complex quantity, characterized by a modulus and a phase Δ = |Δ|eiS .

(16.41)

The phase, in particular, ﬁxes the superﬂuid velocity according to the fundamental identiﬁcation vs = (/2m)∇S, where, with respect to the analogous case holding in atomic BECs (see eqn (6.16)), one should notice the factor 2 which reﬂects the fact that that the relevant constituents responsible for the superﬂuid motion are pairs rather than single atoms. This is true along the whole BCS–BEC crossover.

322

Interacting Fermi Gases and the BCS–BEC Crossover

Another important feature of a superﬂuid Fermi gas is given by its excitation spectrum. In contrast to Bose systems, Fermi superﬂuids exhibit two branches in the excitation spectrum: a fermionic and a bosonic branch. Fermionic excitations possess half-integer spin, like particle and hole excitations in a normal Fermi ﬂuid, and can also be called single-particle excitations. They can only be created in pairs, as a consequence of the fact that the total angular momentum can only be changed by an integer value. However, a fermionic excitation in the superﬂuid is a combination of a particle and a hole, as a consequence of the Bogoliubov transformations and the spontaneous breaking of gauge invariance. As a result, and unlike the normal phase where only colliding particle and hole excitations can annihilate during a collision with the consequent emission of phonons, the annihilation process in a superﬂuid can concern the collision of any pair of excitations. In this sense these excitations are the analogue of neutral Majorana particles of quantum ﬁeld theory (see, for example, Beenakker, 2014). A peculiar feature of Fermi superﬂuids is the occurrence of a gap Δgap in the singleparticle excitation spectrum. At T = 0 this gap is related to the minimum energy required to add or remove one particle starting from an unpolarized system according to the relationship E(N/2 ± 1, N/2) = E(N/2, N/2) ± μ + Δgap . Here, E(N↑ , N↓ ) is the ground state energy of the system with N↑(↓) particles of ↑ (↓) spin, and μ is the chemical potential deﬁned by μ = [E(N/2 + 1, N/2 + 1) − E(N/2, N/2)]/2 = ∂E/∂N . By combining these two relations, one obtains the following expression for the gap: Δgap =

1 [2E(N/2 + 1, N/2) − E(N/2 + 1, N/2 + 1) − E(N/2, N/2)]. 2

(16.42)

The gap corresponds to one half of the energy required to break a pair. The single-particle excitation spectrum, k , is instead deﬁned according to the relation Ek (N/2 ± 1, N/2) = E(N/2, N/2) ± μ + k , where Ek (N/2 ± 1, N/2) denotes the energy of the system with one more (less) particle with momentum k. Since Δgap corresponds to the lowest of such energies Ek , it coincides with the minimum of the excitation spectrum. Near the minimum the spectrum can be represented as 2

k = Δgap +

2 (k − k0 ) . 2m∗

(16.43)

In Section 16.5 we provided the explicit form for k near the Fermi surface, holding in the BCS limit of negative and small values of the scattering length (see eqn (16.18)). In general, the order parameter Δ and the gap Δgap are independent quantities. A direct relationship holds in the weakly attractive BCS regime (see Section 16.5), where one ﬁnds Δgap = Δ. In this regime one also ﬁnds k0 = kF and m∗ = Δ/vF2 . On the BEC side the gap instead coincides with one half of the dimer binding energy: Δgap → 2 /2ma2 . This quantity, for small values of a, is much larger than the critical temperature. Thus, unlike the order parameter it is not always true that the gap vanishes above the critical temperature. On the BEC side bound molecules also exist above the critical temperature, but they are not Bose–Einstein condensed. In this case one ﬁnds k0 = 0 and m∗ = m. At unitarity one instead expects k0 ∼ kF

The Bogoliubov–de Gennes approach to the BCS–BEC crossover

323

and m∗ ∼ m. The role of the gap in characterizing the superﬂuid behaviour will be discussed in Section 19.3. Let us now discuss the behaviour of the bosonic branch of excitations. According to Landau, all neutral superﬂuids exhibit gapless density excitations. These modes are collective excitations and should not be confused with the gapped single-particle excitations of fermionic type discussed above. At small wave vectors they take the form of phonons, propagating at T = 0 with the velocity mc2 = n

∂μ . ∂n

(16.44)

These are the Goldstone sound modes associated with the breaking of gauge symmetry. The phonons are the only gapless excitations in the system and provide the main contribution to the temperature dependence of all thermodynamic functions at low temperatures (kB T Δgap ). For example, the speciﬁc heat C and the entropy S of the uniform gas follow the phonon law C = 3S ∝ T 3 . The existence of phonons in neutral Fermi superﬂuids was noted by Bogoliubov, Tolmachev, and Shirkov (1958b) and by Anderson (1958). They are often referred to as the Bogoliubov–Anderson modes. The description of these density oscillations and of their discretized form, in the presence of harmonic trapping, will be presented in Section 19.1. We ﬁnally notice that single-particle excitations, being created in pairs, give rise to a continuum contribution to the dynamic form factor. However, the presence of the gap results in the existence of a threshold frequency 2Δgap / for their creation and in a singularity in the form factor, giving rise to weakly damped collective oscillations with frequency 2Δgap /, also known as Higgs modes (Volkov et al., 1973; Gurarie, 2009; Scott et al., 2012).

16.8

The Bogoliubov–de Gennes approach to the BCS–BEC crossover

A many-body description of the superﬂuid phase of an interacting Fermi system should account for the correlation eﬀects responsible for the long-range order (16.37) in the two-body correlation functions. There is not at present an exact analytic solution of the many-body problem along the whole BCS–BEC crossover. A useful approximation is provided by the mean-ﬁeld picture based on the Bogoliubov–de Gennes (BdG) equations. These equations can be derived using the formalism of the pseudo-potential developed in Section 9.2 and accounting only for pairing correlations at the mean-ﬁeld level. We will consider here the T = 0 limit and the unpolarized case N↑ = N↓ = N/2. In the absence of external conﬁnement we can write the expression ˆ BCS = H

σ

−

2 2 ˆ σ (r) ˆ † (r) − ∇ − μ Ψ dr Ψ σ 2m

,

ˆ † (r)Ψ ˆ † (r)Ψ ˆ † (r) − 1 Ψ ˆ † (r) + h.c. dr Δ(r) Ψ ↑ ↓ ↓ 2 ↑

(16.45)

324

Interacting Fermi Gases and the BCS–BEC Crossover

for the mean ﬁeld Hamiltonian. The direct (Hartree) interaction term, proportional ˆ ↑ (r) and Ψ ˆ † (r)Ψ ˆ ↓ (r), is neglected in eqn (16.45) in order ˆ † (r)Ψ to the averages Ψ ↑ ↓ to avoid the presence of divergent terms in the theory when applied to the unitary limit 1/a → 0. The order parameter Δ is deﬁned here as the spatial integral of the short-range potential V (s) weighted by the pairing ﬁeld (16.38) Δ(r) = −

ˆ ↓ (r + s/2)Ψ ˆ ↑ (r − s/2) = −g(sF )s=0 , ds V (s)Ψ

(16.46)

where g = 4π2 a/m. The last equality, which is obtained using the pseudo-potential (9.22), is consistent with the deﬁnition of the order parameter given in eqn (16.39). The ˆ † (r)Ψ ˆ † (r)/2 + h.c.) has been included in the Hamiltonian c-number term dr(Δ(r)Ψ ↑ ↓ (16.45) to avoid double counting in the ground state energy, a typical feature of the mean-ﬁeld approach. ˆ ↑ (r) = The Hamiltonian (16.45) is diagonalized by the Bogoliubov transformation Ψ † † ∗ ∗ ˆ ˆ ˆ αi + vi (r)βi ), Ψ↓ (r) = αi ), which transforms particles i (ui (r)ˆ i (ui (r)βi − vi (r)ˆ into quasi-particles denoted by the operators α ˆ i and βˆi . Since quasi-particles should also satisfy the fermionic anti-commutation relations, αi , α ˆ i† } = {βˆi , βˆi† } = δi,i , the {ˆ ∗ functions ui and vi obey the orthogonality relation dr [ui (r)uj (r) + vi∗ (r)vj (r)] = δij . As a consequence of the Bogoliubov transformations the Hamiltonian (16.45) can be written in the form ˆ BCS = (E0 − μN ) + H

ˆ i† α i α ˆ i + βˆi† βˆi ,

(16.47)

i

which describes a system of independent quasi-particles. The corresponding expressions for the amplitudes ui and vi are obtained by solving the matrix equation

H0

Δ(r)

Δ∗ (r)

−H0

ui (r)

vi (r)

= i

ui (r)

,

(16.48)

vi (r)

where H0 = −(2 /2m)∇2 − μ is the single-particle Hamiltonian. The order parameter Δ(r) is in general a complex, position-dependent function. Equation (16.48) is known as the Bogoliubov–de Gennes equation (de Gennes, 1989). It can be used to describe both uniform and nonuniform conﬁgurations like, for example, quantized vortices (see Sensarma et al., 2006) or solitons (Antezza et al., 2007). In the take the simple form of plane waves ui (r) → √ uniform case the solutions √ eik·r uk / V and vi → eik·r vk / V , with u2k

=1−

vk2

1 = 2

ηk 1+ , k

uk vk =

Δ , 2k

(16.49)

The Bogoliubov–de Gennes approach to the BCS–BEC crossover

325

where ηk = 2 k 2 /2m − μ is the energy of a free particle calculated with respect to the chemical potential. The spectrum of quasi-particles, which are the elementary excitations of the system, has the well-known form 2 2 2 k k = Δ2 + −μ , (16.50) 2m and close to the Fermi surface coincides with the result (16.18) holding in the weak coupling BCS limit with Δgap = Δ. In the BCS regime, the minimum of k corresponds to the Fermi wave vector kF . The minimum is shifted towards smaller values of k as one approaches the unitary limit and corresponds to k = 0 when the chemical potential changes sign on the BEC side of the resonance. Furthermore, one should notice that while the BCS theory correctly predicts the occurrence of a gap in the single-particle excitations, it is instead unable to describe the low-lying density oscillations of the gas (Bogoliubov–Anderson phonons). These can be accounted for by a time-dependent version of the theory (see, for example, Urban and Schuck, 2006). The vacuum of quasi-particles, deﬁned by α ˆ k |0 = βˆk |0 = 0, corresponds to the ground state of the system, whose energy is given by 2 k 2 Δ2 E= vk2 − 2 . (16.51) 2m 2k k

The above energy consists of the sum of two terms: the ﬁrst is the kinetic energy of the two spin components, while the second corresponds to the interaction energy. One should notice that both terms, if calculated separately, exhibit an ultraviolet divergence which disappears in the sum, yielding a ﬁnite total energy. The order parameter Δ entering the above equations should satisfy a self-consistent condition determined by the short-range behaviour (16.39) of the pairing ﬁeld (16.38). This function takes the form dk dk eik·s ik·s F (s) = u v e = Δ . (16.52) k k (2π)3 (2π)3 2k By writing (4πs)−1 = dkeik·s /[(2π)3 k 2 ] and comparing eqn (16.39) with eqn (16.52), one obtains the important equation m 1 dk m = , (16.53) − 4π2 a (2π)3 2 k 2 2k the integral of the diﬀerence in the brackets being convergent. Equation (16.53), through the expression (16.50) for the spectrum of the elementary excitations, provides a relationship between the order parameter Δ and the chemical potential μ entering the single-particle energy. A second relation is given by the normalization condition 2 2 ηk dk n= 1 − , (16.54) vk = V (2π)3 k k

326

Interacting Fermi Gases and the BCS–BEC Crossover

which takes the form of an equation for the density. One can prove that the density dependence of the chemical potential arising from the solution of eqns (16.53) and (16.54) is consistent with the thermodynamic relation μ = ∂E0 /∂N , with E0 given by eqn (16.51). It is worth mentioning that result (16.53) can equivalently be derived starting from the contact potential g˜δ(r), rather than from the regularized form (9.22), using the renormalized value 1 m dk m = − (16.55) 2 g˜ 4π a (2π)3 2 k 2 of the coupling constant, corresponding to the low-energy limit of the two-body Tmatrix (Randeria, 1995). In this case one must introduce a cut-oﬀ in the calculation of ˆ ↓Ψ ˆ ↑ = −˜ the order parameter Δ = −˜ g Ψ g dkΔ/[2k (2π)3 ], as well as in the integral in eqn (16.55), in order to avoid the emergence of ultraviolet divergences. In the case of weakly attractive gases (kF |a| 1 with a < 0) the chemical potential approaches the Fermi energy μ EF and eqn (16.53) reduces to the equation for the gap of standard BCS theory. In the general case, the value of μ and Δ should be calculated by solving the coupled equations (16.53) and (16.54). By expressing the energy in units of the Fermi energy EF these equations only depend on the dimensionless parameter 1/kF a which characterizes the interaction strength along the BCS–BEC crossover. In the following we will be referring to eqns (16.48), (16.53) and (16.54) as the Bogoliubov–de Gennes (BdG) mean-ﬁeld equations. Analytical results for the energy per particle are obtained in the limiting cases 1/kF a → ±∞ corresponding, respectively, to the BEC and BCS regimes. In the BCS limit the mean-ﬁeld equations give the result E 3 40 = EF 1 − 4 e−π/kF |a| + . . . , (16.56) N 5 e while in the BEC limit one ﬁnds 2 2 E0 =− nd 2a + . . . . + π N 2ma2 2m

(16.57)

While the leading term in the energy per particle is correctly reproduced in both limits (yielding, respectively, the noninteracting energy 3EF /5 and half of the dimer binding energy b /2 = −2 /2ma2 ), the higher-order terms are wrongly predicted by this approach. In fact, in the BCS limit the theory misses the interaction-dependent terms in the expansion (16.8). This is due to the absence of the Hartree term in the Hamiltonian (16.45). In the BEC limit the theory correctly reproduces a repulsive gas of dimers. However, the comparison with eqn (16.15) shows that the term arising from the interaction between dimers corresponds, in the expansion (16.57), to a molecule– molecule scattering length equal to add = 2a rather than to the correct value add = 0.60a (see Section 21.4). Furthermore, the Lee–Huang–Yang correction in the equation of state of composite bosons (see eqn (16.15)) is not accounted for by the expansion, the ﬁrst correction to eqn (16.57) being of order a4 (see, for example, Giorgini et al., 2008).

The Bogoliubov–de Gennes approach to the BCS–BEC crossover

327

It is worth noticing that the energy per particle, as well as the chemical potential, change sign from the BCS to the BEC regime. This implies that there exists a value of kF a where μ = 0. This fact bears important consequences on the gap Δgap characterizing the spectrum (16.50) of single-particle excitations. If μ > 0, Δgap coincides with the order parameter Δ. This is the case, in particular, in the BCS regime, where one ﬁnds the result

8 π Δgap = Δ = 2 EF exp − . (16.58) e 2kF |a| Notice that result (16.58) does not include the Gorkov–Melik-Barkhudarov correction (see eqns (16.17) and (16.19)). At unitarity one ﬁnds (Randeria, 1995) Δgap = Δ 0.69EF , a value signiﬁcantly larger than the best available estimate Δ ∼ 0.50EF provided by quantum Monte Carlo simulations (Carlson et al. 2003; Carlson and Reddy, 2005). When μ < 0 the gap predicted by the BdG mean ﬁeld theory is instead given by Δgap = Δ2 + μ2 and in the deep BEC √ limit it approaches the value Δgap = μ. In this limit, in fact, Δ = (16/3π)1/2 EF / kF a |μ|. The average single-particle occupation number of either spin species nk = ˆ a†k↑ a ˆk↑ = ˆ a†k↓ a ˆk↓ is another direct output of the BdG mean-ﬁeld theory. For a given value of kF a along the crossover it is readily obtained in terms of the corresponding values of μ and Δ through the expression η 1 k nk = vk2 = 1− 2 . (16.59) 2 ηk + Δ2 In the BCS regime, nk coincides approximately with the step function Θ(1 − k/kF ) characteristic of the noninteracting gas, the order parameter Δ providing only a small broadening around the Fermi wave vector. By increasing the interaction strength the broadening of the Fermi surface becomes more and more signiﬁcant. At unitarity, 1/kF a = 0, the eﬀect is of the order of kF , consistent with the size of Δ being proportional to the Fermi energy (see Section 16.6). In the BEC regime nk instead takes the limiting form nk =

4(kF a)3 , 3π(1 + k 2 a2 )2

(16.60)

which is proportional to the square of the Fourier transform of the molecular wave function (9.24). For large wave vectors the momentum distribution (16.59) decays as nk 1/k 4 . This behaviour has important consequences for the kinetic energy of the system Ekin = 2 k nk 2 k 2 /2m which diverges in two and three dimensions. This unphysical behaviour arises from the use of the zero-range pseudopotential (9.22) which describes correctly only the region of wave vectors much smaller than the inverse eﬀective range of interactions. It reﬂects the fact that, similarly to the case of interacting Bose gases (see Section 4.3), the kinetic energy is a microscopic quantity that cannot in general be expressed in terms of the scattering length and cannot be calculated employing

328

Interacting Fermi Gases and the BCS–BEC Crossover

mean-ﬁeld theories. In Chapter 18 we will discuss this behaviour on a more general basis, providing a link between this asymptotic behaviour and the existence of relevant thermodynamic relations that were recently derived in a series of papers by Tan (2008a,b). Let us ﬁnally mention that a generalization of the BdG equation, based on a density functional approach and accounting for an improved description of the equation of state and of the superﬂuid gap, has been proposed by Bulgac et al. (2012) and employed for systematic time-dependent studies. Let us now brieﬂy discuss the many-body structure of the ground state wave function. The BCS ground state, deﬁned as the vacuum state for the quasi-particles α ˆk and βˆk , can be written explicitly in terms of the amplitudes uk , vk giving the result % uk + vk a (16.61) ˆ†k↑ a ˆ†−k↓ |0, |BCS = k

where |0 is the particle vacuum. It is important to stress that the BdG mean-ﬁeld eqns (16.53) and (16.54) can equivalently be derived from a variational calculation applied to the state (16.61) where the grand canonical energy is minimized with respect to uk , vk , subject to the normalization constraint u2k +vk2 = 1. The BCS state (16.61) does not correspond to a deﬁnite number of particles. In fact, it can be decomposed into a series of states having an even number of particles |BCS ∝ |0+ Pˆ † |0+(Pˆ † )2 |0+. . . , ˆ†k↑ a ˆ†−k↓ is the pair creation operator. By projecting the state where Pˆ † = k vk /uk a (16.61) onto the Hilbert space corresponding to N particles one can single out the component |BCSN ∝ (Pˆ † )N/2 |0 of the series. In coordinate space this N -particle state can be expressed in terms of an antisymmetrized product of pair orbitals (Leggett, 1980): ! ΨBCS (r1 , . . . , rN ) = Aˆ φ(r11 )φ(r22 ) . . . φ(rN↑ N↓ ) . (16.62) Here Aˆ is the antisymmetrizer operator and the function φ(r) = (2π)−3 dk(vk /uk )eik·r depends on the relative coordinate rii = |ri − ri | of the pair of particles, i (i ) being labels for the spin-up (down) particles. It is worth noticing that in the deep BEC regime, corresponding to |μ| 2 /2ma2 Δ, the pair orbital becomes proportional to the molecular wave function (9.24), and the many-body wave function (16.62) describes a system where all atoms are paired into bound molecules. Wave functions of the form (16.62) are used in order to implement more microscopic approaches to the many-body problem (see, for example, Astrakharchik et al., 2004a; Chang et al., 2004).

16.9

Equation of state, momentum distribution, and condensate fraction of pairs

In the preceding sections we discussed several features of the equation of state of an interacting Fermi gas along the BCS–BEC crossover. The mean-ﬁeld picture, based on the BdG equations, provides a comprehensive general description. Its main merit is to provide a continuous picture of the equation of state as a function of a single parameter—the scattering length—and to emphasize the key role played by the

Equation of state, momentum distribution, and condensate fraction of pairs

329

relevant order parameter of the problem, given by the oﬀ-diagonal long-range order characterizing the two-body density matrix in the superﬂuid phase. The mean-ﬁeld theory is, however, inadequate in the description of important details of the problem, and it is consequently interesting to compare in a more systematic way its predictions with more microscopic approaches that have become available in recent years through quantum Monte Carlo simulations. In this section we restrict our discussion to the T = 0 case where more systematic calculations have become available along the crossover. Figure 16.6 shows the energy per particle along the BCS–BEC crossover as a function of the relevant dimensionless parameter 1/kF a. In order to emphasize many-body eﬀects on the BEC side of the resonance, the contribution b /2 of the dimer binding energy has been subtracted from E/N . The ﬁgure shows the predictions of the ﬁxed-node diﬀusion Quantum Monte Carlo (FN-DMC) simulation of Astrakharchik et al. (2004a). In both the BCS and the BEC regimes the calculated energies agree, respectively, with the perturbation expansion (16.8) and (16.15). In particular, the inset in Figure 16.6 shows an enlarged view of the results in the BEC regime, indicating good agreement with the add = 0.60a result for the dimer–dimer scattering length as well as evidence

1.0 0.08 0.07

(E/N– εb/2)/(3EF/5)

0.06

0.8

0.05 0.04

(E/N– εb/2)/(3EF/5)

0.03

0.6

0.02

–1/kF a

0.01 0.00

–6

–5

–4

–3

–2

–1

0.4

0.2

0.0

–6

–4

–2

0 –1/ kF a

2

4

6

Figure 16.6 Energy per particle along the BCS–BEC crossover with the binding-energy term subtracted from E/N . Symbols: quantum Monte Carlo results from Astrakharchik et al. (2004a). The dot–dash line corresponds to the expansion (16.8) and the dashed line to the expansion (16.15) holding, respectively, in the BCS and in the BEC regime. The longdashed line refers to the result of the BdG mean-ﬁeld theory. Inset: enlarged view of the BEC regime −1/kF a ≤ −1. Here the solid line corresponds to the mean-ﬁeld term in the expansion (16.15); the dashed line includes the Lee–Huang–Yang correction. From Giorgini et al. (2008).

330

Interacting Fermi Gases and the BCS–BEC Crossover

for beyond-mean-ﬁeld eﬀects. This region of the equation of state has been explored experimentally by Nascimbene et al., conﬁrming the predictions of the theory, as already discussed in Section 16.4. The mean-ﬁeld results, based on the predictions of the BdG equations (see previous section) reproduce the correct qualitative behaviour, but are aﬀected by important quantitative inadequacies. In particular, both the BEC and BCS regimes are not correctly described by the mean-ﬁeld approach, resulting in visible discrepancies in the comparison shown in the ﬁgure. At unitarity the value of the energy is quenched with respect to the ideal Fermi gas model by the Bertsch parameter ξB . The BdG theory predicts the value 0.59 for ξB , while the FN-DMC result shown in the ﬁgure gives ξB = 0.42. A smaller value (ξB = 0.37) is predicted by the more advanced quantum Monte Carlo approach of Carlson et al. (2011) which overcomes the fermion sign problem exhibited by previous simulations. The quantum FN-DMC and mean-ﬁeld results for single-particle occupation number nk (proportional to the momentum distribution) and for the condensate fraction of pairs ncond are reported in Figures 16.7 and 16.8, respectively (Astrakharchik et al., 2005a). In both cases, the mean-ﬁeld predictions are in reasonable agreement with the ﬁndings of the FN-DMC calculations. Signiﬁcant discrepancies are found in the behaviour of nk at unitarity (see Figure 16.7), where the broadening of the distribution is overestimated by the mean-ﬁeld theory, consistent with the larger value predicted for the pairing gap (Carlson et al., 2003). The momentum distribution in harmonic traps is discussed in Section 17.3. An important remark concerns the condensate fraction ncond deﬁned in eqn (16.40) which, in the BEC regime, is characterized 1.0

0.007

1/kF a = –1 0.8

0.006 0.005 0.004

nk

0.003

0.6

1/ kF a = 0

0.002

k/kF

0.001

nk

0.000 0

1

2

3

4

5

6

0.4

0.2

0.0 0.0

1/ kF a = 1

0.5

1.0 k / kF

1.5

2.0

Figure 16.7 Quantum Monte Carlo results of the single-particle occupation number nk for diﬀerent values of 1/kF a (solid lines). The dashed lines correspond to the mean-ﬁeld results from eqn (16.59). Inset: nk for 1/kF a = 4. The dotted line corresponds to the momentum distribution of the molecular state eqn (16.60). From Giorgini et al. (2008).

Equation of state, momentum distribution, and condensate fraction of pairs

331

1.0

Condensate fraction

0.8

0.6

0.4

0.2

0.0

–4

–3

–2

–1

0 –1/ kF a

1

2

3

4

Figure 16.8 Condensate fraction of pairs ncond (eqn (16.40)) as a function of the interaction strength: FN-DMC results (circles), Bogoliubov quantum depletion of a Bose gas with add = 0.60a (dashed line), BCS theory including the Gorkov–Melik-Barkhudarov correction (dotdashed line), and mean-ﬁeld theory using eqn (16.52) (solid line). From Giorgini et al. (2008).

√ by the Bogoliubov quantum depletion 1 − ncond = 8 nd a3dd /3 π of a gas of interacting composite bosons with density nd = n/2 and scattering length add = 0.60a. This behaviour is indeed demonstrated by the FN-DMC results of Figure 16.8, but is not recovered within the mean-ﬁeld approximation. On the opposite BCS side of the resonance the FN-DMC results agree reasonably well with the condensate fraction (16.40) calculated using the BCS prediction (Bardeen et al., 1957) FBCS (s) =

ΔkF3 sin(kF s) K0 (sξ) F 4π 2 kF s

(16.63)

for the pairing function (16.38), after inclusion of the Gorkov−Melik-Barkhudarov correction in the expression of the gap (Astrakharchik et al., 2004b). Here K0 is the modiﬁed Bessel function and ξ = 2 kF /mΔ id the BCS coherence length. This result is expected to reproduce the correct behaviour of ncond in the deep BCS regime and is signiﬁcantly lower than the mean-ﬁeld prediction (see Figure 16.8). Condensation of pairs has been observed on both sides of the Feshbach resonance by detecting the emergence of a bimodal distribution in the released cloud after the conversion of pairs of atoms into tightly bound molecules using a fast magnetic-ﬁeld ramp (Regal, Greiner, and Jin, 2004b; Zwierlein et al., 2004; Zwierlein et al., 2005a). The magnetic-ﬁeld sweep is slow enough to ensure full transfer of atomic pairs into dimers, but fast enough to act as a sudden projection of the many-body wave function onto the state of the gas far on the BEC side of the resonance. The resulting condensate fraction is an out-of-equilibrium property, whose theoretical interpretation is not straightforward (Perali, Pieri, and Strinati, 2005; Altman and Vishwanath, 2005), but

332

Interacting Fermi Gases and the BCS–BEC Crossover

it strongly supports the existence of ODLRO in the gas at equilibrium also on the BCS side of the Feshbach resonance (negative a) where no stable molecules exist in vacuum. It is worth observing that the condensate fraction should not be confused with the superﬂuid density. As already pointed out in the ﬁrst part of volume, this identiﬁcation is a good approximation only for a weakly interacting Bose gas. At zero temperature the superﬂuid density actually coincides with the total density (see also Figure 16.4), while the condensate fraction can signiﬁcantly deviate from 1 in interacting conﬁgurations. This is the case of superﬂuid Helium where the condensate fraction is less than 10 per cent. In the Fermi gas at unitarity the quantum Monte Carlo calculations reported in Figure 16.8 predict that the condensate fraction of pairs is about 50 per cent. Even smaller fractions are predicted on the BCS side of the resonance where the system asymptotically approaches the ideal Fermi gas and the condensate fraction is exponentially small. Let us ﬁnally mention that Monte Carlo calculations also provide important predictions for other quantities of high physical interest, such as the pair correlation functions in both the density and spin channels. The discussion of these quantities lies outside the scope of this volume (for a general discussion see, for example, Giorgini et al., 2008).

17 Fermi Gas in the Harmonic Trap This chapter deals with Fermi gases conﬁned in harmonic traps. After a summary of some key properties of the harmonically trapped ideal gas (Section 17.1) we focus on the eﬀect of interactions, employing the local density approximation to calculate the density proﬁles and the momentum distribution along the BCS–BEC crossover (Sections 17.2 and 17.3).

17.1

The harmonically trapped ideal Fermi gas

The ideal Fermi gas trapped by a harmonic potential of the form Vho =

1 1 1 mωx2 x2 + mωy2 y 2 + mωz2 z 2 2 2 2

(17.1)

is a model system with many applications in diﬀerent ﬁelds of physics, ranging from nuclear physics to more recent studies of quantum dots. Here, we will mainly focus on the most relevant features of the model, emphasizing the large N behaviour, where many single-particle states are occupied and the semiclassical approach can safely be used. The simplest approach is to use the semiclassical description of the Fermi distribution function for a given spin species: fσ (r, p) =

1 , exp[β (p2 /2m + Vho (r) − μσ )] + 1

(17.2)

where β = 1/kB T and μσ is the chemical potential of each species, ﬁxed by the normalization condition drdp Nσ = fσ (r, p). (17.3) (2π)3 For simplicity, in eqn (17.2) we have assumed that the trapping potential is the same for the two spin species. As in the case of the uniform gas (see eqn (16.3)) one can introduce the single-particle density of states g() whose energy dependence is given, in the case of harmonic trapping, by eqn (10.15). In terms of the density of states one can calculate all the relevant thermodynamic functions. For example, the energy of the Fermi gas is given by the expression ∞ g() E(T ) = . (17.4) d β(−μ) e +1 0

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

334

Fermi Gas in the Harmonic Trap

At T = 0 the chemical potential μ coincides with the Fermi energy EFho ≡ kB TFho = (6Nσ )1/3 ωho ,

(17.5)

where ωho = (ωx ωy ωz )1/3 is the geometrical average of the three trapping frequencies and the energy takes the value E(0) = (3/4)EFho Nσ . It is worth noting that the Fermi energy (17.5) has the same dependence on the number of trapped atoms and on the oscillator frequency ωho as the critical temperature for Bose–Einstein condensation (see eqn (10.10)) and provides a typical scale of energy (and hence of temperature) for the emergence of quantum degeneracy eﬀects. Another important quantity to investigate is the release energy Erel deﬁned as the energy of the gas after a sudden switch-oﬀ of the conﬁning potential. In the ideal Fermi gas model it coincides with the kinetic energy. The release energy is directly accessible in time-of-ﬂight experiments and, as a consequence of the equipartition theorem applied to the ideal gas with harmonic conﬁnement, is equal to Erel = E/2, where E(T ) is the total energy (17.4). At low T the energy per particle deviates from the classical value 3kB T due to quantum statistical eﬀects, as clearly demonstrated in the JILA experiment (DeMarco and Jin, 1999; DeMarco, Papp, and Jin, 2001) reported in Figure 17.1. The Fermi energy (17.5) can be used to deﬁne typical length and momentum scales characterizing the Fermi distribution in coordinate and momentum space, respectively. The radii # ωho Ri = 2EFho /mωi2 = aho (48Nσ )1/6 , (17.6) ωi

2.0 mf = 9/2 E/3kBT

1.8 1.6 mf = 7/2

1.4 1.2 1.0 0.0

0.5

1.0

1.5

T/TF

Figure 17.1 Evidence for quantum degeneracy eﬀects in trapped Fermi gases. The average energy per particle, extracted from absorption images, is shown for two-spin mixtures. In the quantum degenerate regime the data agree well with the ideal Fermi gas prediction (solid line). The horizontal dashed line corresponds to the result of a classical gas. From DeMarco c 2001, et al. (2001). Reprinted with permission from Physical Review Letters, 86, 5409; American Physical Society.

The harmonically trapped ideal Fermi gas

335

also called Thomas Fermi radii, where aho = /mωho , give the width of the density distribution at T = 0, which can be calculated by integrating the distribution function in momentum space: nσ (r) =

2 2 2 3/2 Nσ x dp 8 y z 1− fσ (r, p) = 2 − − . (17.7) 3 (2π) π Rx Ry Rz Rx Ry Rz #

The Fermi momentum pF = distribution nσ (p) =

2mEFho instead ﬁxes the width of the momentum

2 3/2 8 Nσ p dr 1− fσ (r, p) = 2 3 3 (2π) π (pF ) pF

(17.8)

obtained by integrating the T = 0 distribution function in coordinate space. The Fermi momentum permits us to deﬁne the Fermi wave vector kF0 =

1 pF = (48)1/6 Nσ1/6 , aho

(17.9)

which will often be employed as a useful inverse length scale. Equations (17.7) and (17.8), which are normalized to the total number of particles Nσ , hold for positive values of their arguments and are often referred to as the T = 0 Thomas–Fermi distributions. Equation (17.8) is the analogue of the most familiar momentum distribution 3Nσ /(4πp3F ) Θ(1 − p2 /p2F ) characterizing a uniform Fermi gas in terms of the Fermi momentum pF . The broadening of the Fermi surface with respect to the uniform case is the consequence of harmonic trapping. Notice that the value of kF0 deﬁned above coincides with the Fermi wave vector kF0 = [6π 2 nσ (0)]1/3 calculated for a uniform gas with the central density nσ (0). It is worth comparing eqns (17.7) and (17.8) with the analogous results holding for a trapped Bose–Einstein condensed gas in the Thomas–Fermi limit (see Section 11.3). The shapes of the Fermi and Bose proﬁles do not look very diﬀerent in coordinate space. In both cases the radius of the atomic cloud increases with N , although the explicit dependence is slightly diﬀerent (N 1/5 for bosons and N 1/6 for fermions). Notice, however, that the form of the density proﬁles has a signiﬁcantly diﬀerent physical origin in the two cases; for bosons it is ﬁxed by the repulsive two-body interactions, while in the Fermi case is determined by the quantum pressure. In momentum space, however, the Bose and Fermi distributions diﬀer in a profound way. First, as a consequence of the semiclassical picture, the momentum distribution of the Fermi gas is isotropic even if the trapping potential is deformed (see eqn (17.8)). This behaviour diﬀers from what happens in the BEC case, where the momentum distribution is given by the square of the Fourier transform of the condensate wave function and is hence sensitive to the anisotropy of the conﬁnement (see eqn (11.18)). Second, the width of the momentum distribution of a trapped Bose–Einstein condensed gas decreases with increasing N while, according to eqns (17.8) and (17.9), the momentum width of a trapped Fermi gas increases with the number of particles.

336

Fermi Gas in the Harmonic Trap

It is ﬁnally useful to calculate the time evolution of the density proﬁle after turning oﬀ the trapping potential. For a noninteracting gas, the distribution function follows the ballistic law f (r, p, t) = f0 (r − pt/m, p), where f0 is the distribution function at t = 0 given by (17.2). By integrating over p one can easily calculate the time evolution of the density and one ﬁnds the following result for the mean square radii (i = x, y, z): ri2 =

E(T ) 1 (1 + ωi2 t2 ). Nσ 3mωi2

(17.10)

The asymptotic isotropy predicted by eqn (17.10) is the consequence of the absence of collisions during the expansion and reﬂects the isotropy of the momentum distribution (17.8).

17.2

Equation of state and density proﬁles

In Chapter 16 we discussed the interaction eﬀects in a uniform Fermi gas. These results provide a useful tool for investigating the behaviour of the gas in conditions of external trapping, thanks to the use of the local density approximation (LDA). The LDA is based on the assumption that, locally, the system can be treated as a piece of uniform matter (see also the discussion in Section 13.6). This means that the chemical potential μ0 of the trapped gas can be calculated using the expression μ0 = μ(n, T ) + Vho (r),

(17.11)

where μ(n, T ) is the chemical potential of uniform matter calculated for a ﬁxed value of density and temperature. We have here considered the case of equal numbers of atoms in each atomic species and assumed equal trapping potentials. Equation (17.11) provides an implicit equation for the density n(r, T ), the chemical potential μ0 being ﬁxed by the normalization condition dr n(r, T ) = N . The LDA is expected to be a reliable approximation for suﬃciently large systems where ﬁnite-size corrections and gradient terms in the density proﬁle are small. While in the case of Bose–Einstein condensed gases this condition is ensured by the repulsive interaction among atoms, in the Fermi case the situation is diﬀerent. In fact, thanks to the quantum pressure term related to the Pauli principle, even in the noninteracting case one can apply the LDA relationship (17.11) and one recovers directly the result (17.7) for the density distribution of the noninteracting Fermi gas. Interactions modify the shape and size of the density proﬁle. A simple result is obtained at unitarity at zero temperature where the chemical potential of uniform matter (μ = ξB (2 /2m)(3π 2 n)2/3 ) has the same density dependence as the ideal Fermi gas, apart from the dimensionless Bertsch factor ξB accounting for the interactions (see Section 16.6). By dividing eqn (17.11) by ξB , one ﬁnds that the T = 0 results at unitarity are obtained from those of the ideal Fermi gas simply by √ rescaling the trapping frequencies and the chemical potential according to ωi → ωi / ξB and μ0 → μ0 /ξB . In particular, the density proﬁle at unitarity takes the same form (17.7) as in the ideal gas, the Thomas–Fermi radii being given by the rescaled law ωho 1/4 1/4 Ri = ξB Ri0 = ξB aho (24N )1/6 . (17.12) ωi

Equation of state and density proﬁles

337

1/2

0 From the above results one also ﬁnds the useful expression Eho = ξB Eho for the oscillator energy Eho = drVho n(r) (17.13)

0 = (3/8)N EFho . of the trapped gas in terms of the ideal gas value Eho In the BCS regime, where a is negative and small, the eﬀects of pairing are exponentially small and the ﬁrst correction to the noninteracting density proﬁle (17.7) can be calculated using perturbation theory. The ﬁrst correction to the energy of uniform matter has the same form as for a weakly repulsive Fermi gas (see eqn (16.5)) and the corresponding correction to the local chemical potential is negative and takes the form 4π2 an/2m. The resulting density proﬁle is compressed with respect to the ideal gas prediction and the Thomas–Fermi radii reduce according to the law 256 0 0 Ri = Ri 1 + k a , (17.14) 315π 2 F

which holds if kF0 |a| 1, where kF0 is the Fermi wave vector (17.9) of the noninteracting gas. The above discussion shows that the Thomas–Fermi radii are reduced with respect to the ideal Fermi gas prediction both at unitarity and in the BCS regime, reﬂecting the attractive nature of the potential. Another interesting case is the BEC limit, where one treats the interaction between dimers using the mean-ﬁeld term μd = gd n/2 in the equation of state. The coupling constant gd = 2π2 add /m is ﬁxed by the molecule–molecule scattering length add = 0.60a. In this limit the density is given by the typical inverted parabola proﬁle (11.7) of BEC gases and the Thomas–Fermi radii reduce to Ri = aho

15 add N 2 aho

1/5

ωho . ωi

(17.15)

In Figure 17.2 we show the ﬁrst measurements obtained by Bartenstein et al. (2004a) for the in situ density proﬁles in the presence of a harmonically trapped Fermi gasat low temperatures. The plotted proﬁle is the doubly integrated density n(1) (z) = dxdy n(r), corresponding to the quantity measured in the experiment. The attractive nature of the interactions at unitarity is explicitly revealed by the comparison of the width in the BCS regime, where the density proﬁle approaches the ideal Fermi gas shape. At unitarity, where theory predicts n(1) (z) =

N 16 Rz 5π

1−

z2 Rz2

5/2 ,

(17.16)

with Rz given by eqn (17.12), a best ﬁt to the experimental points yields the value ξB ∼ 0.3 for the Bertsch parameter. More accurate values of ξB have now become available (see Section 16.6).

338

Fermi Gas in the Harmonic Trap

1.6

Linear density [1000/μm]

809 G

850 G

882 G

1.2

0.8

0.4

0.0

0

100

200

300 0

100 200 Position [μm]

300 0

100

200

300

Figure 17.2 Experimental results of the double-integrated density proﬁles along the BCS– BEC crossover for a gas of 6 Li atoms. The results at 850 G correspond to unitarity, while those at 809 G and 882 G correspond respectively to the BEC and BCS sides of the resonance. The continuous curve at unitarity is the best ﬁt based on eqn (17.16). The dashed lines correspond to the predictions for a noninteracting gas. From Bartenstein et al. (2004a). Reprinted with c 2004, American Physical Society. permission from Physical Review Letters, 92, 120401;

Understanding the behaviour of the density proﬁles of interacting fermions at ﬁnite temperatures does, of course, require more elaborated procedures. In the BEC regime of small and positive scattering lengths, however, the situation is relatively simple because of the emergence of a typical bimodal distribution characterized by a narrow Bose–Einstein condensate of molecules surrounded by a broader cloud of thermal molecules. The experimental observation of this bimodal distribution, which was actually measured after expansion via time-of-ﬂight measurements (Greiner, Regal, and Jin, 2003; Bartenstein et al., 2004a; Zwierlein et al., 2003; Bourdel et al., 2004; Partridge et al., 2005), represents the most spectacular and direct evidence of the emergence of Bose–Einstein condensation in an interacting Fermi gas (see Figure 1.2). In this BEC regime the critical temperature for the superﬂuid transition is given by the well-known expression kB TBEC = ωho [Nd /ζ(3)]1/3 , where Nd = N/2 is the number of dimers and ζ(3) 1.202. In terms of the Fermi temperature (17.5) of the harmonic oscillator model this result reads ho TBEC = 0.52TFho .

(17.17)

Due to large interaction eﬀects in the superﬂuid and in the thermal cloud, the bimodal structure becomes less and less pronounced as one approaches the resonance,

Momentum distribution

339

and consequently it becomes more diﬃcult to reveal the normal–superﬂuid phase transition looking at the density proﬁle. The temperature dependence of the thermodynamic functions of a Fermi gas in a harmonic trap along the crossover has been calculated in a series of papers using self-consistent many-body approaches (see the review book edited by Zwerger (2012) and references therein). The most recent predictions, based on the use of LDA and advanced many-body approaches in uniform matter, provide the value kB Tcho = (0.20 ÷ 0.22)EFho

(17.18)

for the critical temperature of the unitary Fermi gas in a harmonic trap (Burovski et al., 2006b; Haussmann and Zwerger (2008); Hu et al. (2008).

17.3

Momentum distribution

The momentum distribution of ultracold Fermi gases is another important quantity carrying a wealth of information on the role played by interactions. A simple approach for trapped systems is based on the local density approximation (Viverit et al., 2004). The result is given by the spatial integral of the particle distribution function nk (r) of the uniform gas dr nk (r), (17.19) n(k) = (2π)3 where the r-dependence enters through the local value of the density n(r) which ﬁxes, at a given temperature, the value of the particle distribution function nk (r). For example, in the case of the mean-ﬁeld description developed in Section (16.8) at zero temperature, through the use of the Bogoliubov–de Gennes equations, the particle distribution function takes the form (16.59). Two limiting cases can be derived analytically: one corresponds to the noninteracting gas, where nk (r) = Θ[1 − k/kF (r)] depends on the local Fermi wave vector kF (r) = [3π 2 n(r)]2/3 and the integral (17.19) yields the result (17.8) for the momentum distribution n(k). The other corresponds to the deep BEC regime, where result (16.60) holds and the atomic momentum distribution is unaﬀected by the trapping potential, being given by the expression n(k) = (a3 N/2π 2 )/(1 + k 2 a2 )2 of a free gas of molecules. A general feature emerging in both cases is the broadening of the momentum distribution with respect to the uniform ideal Fermi gas model caused, in the ﬁrst case by the conﬁnement and, in the second case, by interaction eﬀects. The momentum distribution has been measured along the crossover in a series of studies (Regal et al., 2005; Chen et al., 2006; Tarruell et al., 2007). The ∞ accessible quantity in experiments is the column-integrated distribution ncol (k⊥ ) = −∞ dkz n(k), # where k⊥ = kx2 + ky2 . These experiments are based on the technique of time-of-ﬂight expansion followed by absorption imaging. A crucial requirement is that the gas must expand freely without any interatomic force. To this purpose the scattering length is set to zero by a fast magnetic-ﬁeld ramp immediately before the expansion. The measured column-integrated distributions along the crossover from Regal et al. (2005)

340

Fermi Gas in the Harmonic Trap 1.0

ncol(k)(kF0)2 N

0.8

0.6

0.4

0.2

0.0 0.0

0.5

1.0 k / kF0

1.5

2.0

Figure 17.3 Column-integrated momentum distributions of a trapped Fermi gas. The circles correspond to the experimental results from Regal et al. (2005) and the lines to the meanﬁeld results based on eqn (17.19) for the same values of the interaction parameter 1/kF0 a. From top to bottom these are: 1/kF0 a = −71, 1/kF0 a = 0, and 1/kF0 a = 0.59. From Giorgini et al. (2008).

are shown in Figure 17.3, together with the mean-ﬁeld calculations of ncol based on eqn (17.19) for the same values of the interaction strength 1/kF0 a, the value of a being the scattering length before the magnetic-ﬁeld ramp. There is an overall qualitative agreement between the theoretical predictions and the experimental results, although a quantitative comparison between theory and experiment should take into account the time dependence of the scattering length associated with the dynamics of the magnetic-ﬁeld ramp (Chiofalo et al., 2006). In the next chapter we will discuss how the behaviour of the momentum distribution of a harmonically trapped Fermi gas at high momenta can be used to extract the contact, a key parameter characterizing the thermodynamic behaviour of interacting Fermi gases.

18 Tan Relations and the Contact Parameter This chapter is devoted to illustrating various thermodynamic relations, known as Tan relations, involving the so-called contact parameter. This physical quantity, which determines the behaviour of the momentum distribution of an interacting gas at large momenta (Section 18.2), plays a crucial role in characterizing various thermodynamic quantities, like the dependence of the energy on the scattering length (sweep theorem, Section 18.3), the relation between the energy and the momentum distribution (Section 18.4), the behaviour of the static structure factor at large wave vectors (Section 18.5), and the virial theorem in the presence of harmonic trapping (Section 18.6).

18.1

Wave function of a dilute Fermi gas near a Feshbach resonance

As already anticipated, Fermi gases near a Feshbach resonance exhibit unique manybody properties. In fact, the gas can be dilute in the sense that the average distance d ∼ n−1/3 between atoms is much larger than the range r0 of the force ﬁxed by the atomic size, i.e. n−1/3 r0 . At the same time the interaction can be strong, in the sense that the scattering length can be of the order (or even larger) of the interatomic distances. The calculation of the macroscopic properties of the system in such conditions requires the solution of a diﬃcult many-body problem. However, simple and important relationships can be derived (Tan, 2008a, b) which connect the microscopic behaviour of the wave function at short distances r n−1/3 with its macroscopic behaviour, including the dependence of the equation of state on the value of the scattering length. We will derive the Tan relations for a non-polarized system of fermions occupying two spin states. Similar relations can be derived for polarized systems and fermionic mixtures with diﬀerent masses. More exhaustive discussions concerning the derivation of the Tan relations can be found in the review paper by Braaten (2012). Let us write the wave function of the system in the form Ψ = Ψ(r1↑ , r2↑ . . . rN ↑ ; r1↓ , r2↓ . . . rN ↓ ),

(18.1)

where N =N/2 is the number of fermions in one of the two spin states and N is the number of atoms. The function Ψ is antisymmetric with respect to permutations of

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

342

Tan Relations and the Contact Parameter

the spatial coordinates of two fermions occupying the same spin state. It is assumed to be normalized according to the condition 2 |Ψ| dr1↑ , . . . drN ↑ dr1↓ , . . . drN ↓ = 1. (18.2) The wave function of a stationary state satisﬁes the usual Schr¨ odinger equation: 2 2 2 ∇2i↑ − ∇k↓ + V (|ri↑ − rk↓ |) Ψ = EΨ − (18.3) 2m 2m i↑,k↓

where V (r) is the two-body interaction potential and only interactions between atoms of diﬀerent spins are taken into account. This model describes in the proper way the behaviour of the system in the presence of a Feshbach resonance (see Section 16.7). The central point of Tan’s approach is the behavior of the many-body wave function of an interacting Fermi gas when the distance r = |r1↑ − r1↓ | between two particles of opposite spin (we have chosen here i = k = 1 without any loss of generality) satisﬁes the condition r n−1/3 . In this region the many body wave function (18.1) can be presented in the form Ψ ≈ φ (|r1↑ − r1↓ |) Φ(r2↑ . . . rN ↑ ; r2↓ . . . rN ↓ )

(18.4)

the wave function φ satisfying the two-body Schr¨ odinger equation with zero energy (see (9.14)): −

2 2 ∇ φ + V (r)φ = 0. m r

(18.5)

For r r0 , where on can ignore the interaction potential, the function φ takes the simple form (see eqn (9.21)): φ=

1 1 − . r a

(18.6)

It is worth discussing more carefully the conditions of applicability of eqn (18.6). For negative values of the scattering length expression, (18.6) holds provided r n−1/3 . In the case of positive values of the scattering length, giving rise to a Feshbach molecule, it instead requires the additional condition r a. This can be easily understood in the deep BEC regime of the crossover where the gas can be approximated as a gas of dimers whose wave function e−r/a /r coincides with (18.6) only for r a.

18.2

Tails of the momentum distribution

In this section we will investigate the asymptotic behaviour of the momentum distribution n(k) for momenta much larger than the average momentum of atoms. For a degenerate Fermi gas this corresponds to considering values of |k| such that r0−1 |k| n1/3 ,

(18.7)

Tails of the momentum distribution

343

where the behaviour of n(k) is determined by the region in coordinate space where the wave function takes the form (18.4, 18.6). If the scattering length is positive and we are close to a Feshbach resonance, one should satisfy the additional condition k 1/a (see discussion after eqn (18.6)). Let us rewrite the wave function in the ‘mixed’ representation: Ψ (k1↑ ; r2↑ . . . rN ↑ ; k1↓ ; r2↓ . . . rN ↓ ) = (18.8) dr1↑ dr1↓ Ψ(r1↑ , r2↑ . . . rN ↑ ; r1↓ , r2↓ . . . rN ↓ ) exp [−i (k1↑ · r1↑ + k1↓ · r1↓ )] 3 . (2π) A simple calculation gives

dr↑ dr↓ φ (|r↑ − r↓ |) exp [−i (k↑ · r↑ + k↓ · r↓ )] 3 (2π) 4π = δ (k↑ + k↓ ) φ(r) exp [−i (k↑ · r)] dr = δ (k↑ + k↓ ) 2 , k↑

(18.9)

where we have omitted an inessential contribution arising from the 1/a term of (18.6) and, for simplicity, we have omitted the suﬃx ‘1’. The many-body wave function (18.8) then takes the form Ψ(k↑ ; r2↑ . . . rN ↑ ; k↓ ; r2↓ . . . rN ↓ ) = δ (k↑ + k↓ )

4π Φ. k↑2

(18.10)

2

We are interested in the quantity W = |Ψ(k↑ , . . . .r N ↓ )| , providing the probability in the space {k↑ , r2↑ . . . rN ↑ , k↓ , r2↓ . . . rN ↓ }. This quantity involves the square of the 2 delta function that can be written in the form [δ (k↑ + k↓ )] = V /((2π)3 )δ (k↑ + k↓ ), where V is the volume of the gas. The momentum distribution of the spin-‘up’ particles, which we are looking for, can be obtained by integration over all the variables except k↑ . We should also include the factor N 2 giving the number of pairs of opposite spin. In conclusion, the momentum distribution, satisfying the normalization condition N n(k↑ )dk↑ = , (18.11) 2 for large values of k↑ takes the form N2 1 VC W dk↓ , dr2↑ . . . drN ↓ = n (k↑ ) = , 4 (2π)3 k↑4 where we have deﬁned the ‘contact’ (Tan, 2008a) N2 2 |Φ| dr2↑ , . . . drN ↑ dr2↓ , . . . drN ↓ . C = 16π 2 4

(18.12)

(18.13)

The momentum distribution of the spin-down particles is given by the same equation. The quantity C is an intensive quantity and is also called the homogeneous or local

344

Tan Relations and the Contact Parameter

contact. It should not be confused with the total contact I (see eqn (18.40)) which is the integral of the local contact and is relevant for nonuniform conﬁgurations. So far we have considered a state with a given energy. At ﬁnite temperatures one should average with respect to the Gibbs distribution. This results in the simple 2 2 replacement |Φ| → |Φ| . The explicit calculation of the contact (18.13) requires the knowledge of the manybody wave function Ψ beyond the asymptotic regime of short distances and cannot be carried out in an analytic way. However, as we will show in the following sections, other important observables can be expressed in terms of the same contact parameter. This provides important connections between diﬀerent physical quantities.

18.3

Dependence of energy on scattering length

In this section we will derive an important relation between the derivative of the energy of the gas with respect to the scattering length and the contact parameter (18.13). Let us consider two wave functions of the gas, Ψ and Ψ , corresponding to two diﬀerent values a and a of the scattering length and, correspondingly, to two diﬀerent values E and E of the energy. Let us multiply equation (18.3) by Ψ∗ and the corresponding equation for Ψ∗ by Ψ. By taking the diﬀerence between the two resulting expressions, and noticing that the terms containing the interaction potential exactly cancel out, we obtain ⎡ ⎤ ∗ 2 ⎣ − ∇i↑ · Ψ ∇(i↑) Ψ − Ψ∇i↑ Ψ∗ + ∇k↓ · Ψ∗ ∇k↓ Ψ − Ψ∇(k↓) Ψ∗ ⎦ 2m i↑

= (E − E ) Ψ∗ Ψ.

k↓

(18.14)

Let us now integrate equation (18.14) on the whole coordinate space, excluding the spheres of a small radius ε around the points where the coordinates of atoms with diﬀerent spins coincide, i.e. the spheres deﬁned by |ri↑ − rk↓ | ≤ ε where the wave function φ(|ri↑ − rk↓ |) exhibits the short-range behaviour (18.6). This corresponds to considering N 2 small spheres, each responsible for the same contribution to the integral. By introducing for each of these atomic pairs the new variables r = r1↑ − r1↓ and R = (r1↑ + r1↓ ) /2, where without any loss of generality we have set i = k = 1, the integral of eqn (18.14) can be written in the form 2 2 − N drdRdr2↑ , . . . drN ↑ dr2↓ , . . . drN ↓ 4m r r0 we can safely use the asymptotic expression (18.4) for Ψ. We then get N2 2 φ∗ (r) V (r) φ (r) dr |Φ| dr2↑ , . . . drN ↓ , Eint = V (18.31) 4 where the function φ can safely be replaced with the zero-energy solution of the twobody Schr¨ odinger eqn (18.5). By using for V (r) the pseudopotential V = gδ(r)(∂/∂r)r, with g = 4π2 a/m (see eqn (9.22)), we ﬁnd

1 1 4π2 dr δ(r) − φ∗ (r) V (r) φ (r) dr = − m r a 1 dk 4π2 16π 2 2 , (18.32) + =− 3 m k 2 (2π) ma we have used the momentum representation of the delta function: δ (r) = where e−ik·r dk/(2π)3 . By substituting the above result in (18.31) and comparing with deﬁnition (18.13) for the contact we ﬁnally obtain the convergent result

2 1 VC 2 2 k↑ n (k↑ ) − (18.33) E= dk + V C ↑ 3 4 m 4πma (2π) k↑ for the total energy Ekin + Eint (Tan, 2008a), where, for the sake of clarity, we have restored the suﬃx ↑. One can check this equation for a system of two atoms, using the results E = −2 /(ma2 ) for the energy, C = 4πn/a for the contact and eqn (16.60) for the momentum distribution (n(k↑ ) = V /(2π)3 nk↑ ).

18.5

Static structure factor

Interactions near resonance are responsible for an enhancement of the density correlations between spin-up and spin-down particles. We are interested in the spin-up–down structure factor 1 S↑↓ (q) = dr↑ dr↓ n(2) (r↑ , r↓ ) − n↑ n↓ eiq·(r↑ −r↓ ), (18.34) N

Static structure factor

349

which generalizes the usual density structure factor (7.40) and which exactly vanishes in the noninteracting Fermi gas model. The corresponding spin up–down two-body density matrix is deﬁned by n(2) (r↑ , r↓ ) =

N2 4

2

|Ψ(r↑ , r2↑ . . . ; r↓ , r2↓ . . .)| dr2↑ . . . dr2↓ . . . drN ↓ ,

(18.35)

the factor N 2 /4 accounting for the proper normalization n(2) (r↑ , r↓ ) dr↑ . . . dr↓ = N 2 . In the short-range domain, where we can use the asymptotic behaviour (18.4)–(18.6), we can write (apart from a trivial constant term) n(2) (r↑ , r↓ ) =

C C 2 |φ (r↑ − r↓ )| = 2 16π 16π 2

1 2 , − r2 ar

(18.36)

where r = |r↑ − r↓ |. Performing the Fourier transform, we ﬁnd that the structure factor exhibits, at large q, the following asymptotic behaviour: 4 C 1 − . (18.37) S↑↓ (q) = 8n q πaq 2 Since the structure factors S↑↑ (q) = S↓↓ (q) relative to particles with the same spin do not contain the singular terms (18.37) and in the considered region of large wavevectors 2.2 2.0 1/kF a = 4

1.8

1/kF a = 2

1.6

1/kF a = 1

1.4 1/kF a = 0 1/kF a = –1

S(q)

1.2 1.0

noninteracting gas

0.8 0.6 0.4 0.2 0.0

0

2

4

6 q/ kF

8

10

12

Figure 18.1 Homogeneous static structure factor S(q) for diﬀerent values of the interaction strength, as a function of k/kF . Solid lines correspond to QMC results and dashed lines to the predictions of the BdG mean-ﬁeld theory. The lowest line refers to the noninteracting gas. From Combescot et al. (2006a).

350

Tan Relations and the Contact Parameter

can be taken equal to 1/2, one then ﬁnds that the asymptotic behaviour of the total structure form factor is given by C 1 4 S(q) = 1 + − . (18.38) 8n q πaq 2 Quantum Monte Carlo results for the q dependence of the static structure factor are reported in Figure 18.1, showing explicitly the decrease of S(q) at large q, as predicted by eqn (18.38). It is instructive to compare result (18.38) for the structure factor with the predic−2 tion S(q) √ = 1 − (qξ) of Bogoliubov theory for weakly interacting Bose gases, where ξ = 1/ 8πan is the healing length (see eqn (7.98)). The applicability of Bogoliubov theory requires the condition qa 1 and in this regime the leading term in (18.38) is provided by the 1/q 2 term, in agreement with the Bogoliubov expansion of S(q) (see result (18.28) for the contact).

18.6

The contact of a harmonically trapped gas

In the presence of harmonic traps one can introduce the concept of total contact, by looking at the high-k behaviour of the momentum distribution of the trapped gas which still exhibits a 1/k 4 behaviour, as in uniform systems: n (k↑ ) =

1 I . (2π)3 k↑4

(18.39)

The coeﬃcient of proportionality is called the total contact and is related to the local contact parameter C introduced in Section 18.2, by the integral relation I = drC[n(r)] , (18.40) based on the local density approximation (LDA). For example, at unitarity one has C = αkF4 at T = 0 with kF (r) = [3π 2 n(r)]1/3 (see eqn (18.25)). Here, n(r) is the Thomas– Fermi density ﬁxed by LDA relationship (17.11) with μ = ξB (2 /2m)(3π 2 n)2/3 (see Chapter 17). A simple integration gives (Li and Stringari, 2011; Hoinka et al., 2013) I=

256π αN kF0 . 35 ξ 1/4

(18.41)

B

with the Fermi momentum calculated according to eqn (17.9). In terms of the total contact I one can derive various thermodynamic relations (Tan, 2008b)) which are the analogues of the ones derived in the previous section for a homogeneous gas, as well as a new formulation of the virial theorem which makes explicit use of the scaling properties of the harmonic potential. Let us ﬁrst consider the sweep theorem. In the presence of harmonic trapping the total contact (18.20) is related to the derivative of the total energy with respect to the inverse scattering length. ∂E ∂A 2 I, (18.42) = =− ∂(1/a) S,N ∂(1/a) T,N 4πm

The contact of a harmonically trapped gas

351

where the energy E = Ekin + Eint + Eho

(18.43)

now includes the additional oscillator potential (17.13). The quantity Erel = Ekin + Eint = dr[n(r)],

(18.44)

given by the sum of the kinetic and interaction energies, is called the release energy. It plays an important role experimentally since it coincides with the energy of the expanding gas after switching oﬀ the conﬁning trap and is measurable with time-of-ﬂight techniques. It is a quantity conserved during the expansion and was ﬁrst measured along the crossover by Bourdel et al. (2004) on a gas of 6 Li atoms. It is worth noting that the two contributions to Erel always enter together in the determination of the relevant thermodynamic relations. Actually, in the BdG approach the two contributions separately diverge (see Section 16.8) and only the sum is a well-deﬁned quantity, ﬁxed by the scattering length. The oscillator energy Eho (see eqn (17.13)) is also an experimentally accessible quantity that can be determined through the in situ measurement of the density proﬁle. 5 Momentum rf lineshape PES

I/(N k0F)

4 3 2 1 0 –3

–2

–1

0

(k0F a)–1 Figure 18.2 Measured total contact I as a function of (kF0 a)−1 using three diﬀerent methods. Filled circles correspond to direct measurements of the fermion momentum distribution n(k) using a fast magnetic-ﬁeld sweep to project the many-body state onto a noninteracting state. The momentum distribution can then be measured in ballistic expansion. Open circles correspond to n(k) obtained using atom photoemission spectroscopy measurements. Stars correspond to the contact obtained from rf spectroscopy. The values obtained with these diﬀerent methods show good agreement. The contact is nearly zero for a weakly interacting Fermi gas with attractive interactions (left-hand side of plot) and then increases as the interaction strength increases to the unitarity regime where (kF0 a)−1 = 0. The line is a theory curve obtained from Werner et al. (2009). From Stewart et al. (2010). Reprinted with c 2010, American Physical Society. permission from Physical Review Letters, 104, 235301;

352

Tan Relations and the Contact Parameter

A novel thermodynamic relationship holding in the presence of harmonic trapping is given by the virial theorem. This theorem provides the relationship 2Erel − 2Eho = −

2 I 4πm a

(18.45)

between the release energy, the oscillator energy, and the contact. The virial theorem (18.45) can be derived by applying the number-conserving transformation n(r) → (1 + α)3 n[(1 + α)r] to the density of the gas at equilibrium. By imposing that the variation of the free energy A = f dr vanishes to ﬁrst order in α and writing the free energy density as f = ( − T s) = (2 )/m)n5/3 f˜(T /TF , na3 ), where f˜ is a dimensionless function of the parameters T /TF and na3 , use of simple thermodynamic relationships yields result (18.45). At unitarity, where a → ∞, the virial theorem reduces to the relationship Erel = Eho and was checked experimentally by Thomas et al. (2005). In the Thomas–Fermi limit of a weakly interacting harmonically trapped Bose gas at T = 0, one instead ﬁnds a∂E/∂a = (2/5)E = (2/5)(Eho + Eint ) and hence the result 3Erel = 2Eho , already derived in Section 11.3. The contact was measured in interacting Fermi gases, along the BCS–BEC crossover, in a series of experiments at zero as well as at ﬁnite temperatures. Figure 18.2 20

/ ( NkF0 )

15

10

5

0

QMC + LDA NSR + LDA exp, Kuhnle et al. exp, Hoinka et al.

–1

0 1 / (kF0a)

1

Figure 18.3 Total contact parameter as a function of (kF0 a)−1 . The solid line is obtained from QMC data combined with the LDA, and the dotted line is a Nozi`eres–Schmitt-Rink (NSR) calculation by Hu et al. (2011). The grey squares are experimental data from Kuhnle et al. (2011) obtained from the measured large-k behavior of the structure factor. At unitarity, the experimental result is I/N kF0 = 3.06 ± 0.08, compared with the QMC value: 3.336, and NSR result: 3.26 (Hu et al., 2011). At kF0 a = 0.93 the experiment yields 11.9 ± 0.3, while the QMC and NSR values are ∼ 12.35 (Hu et al., 2011). From Hoinka et al. (2013). Reprinted with c 2013, American Physical Society. permission from Physical Review Letters, 110, 055305;

The contact of a harmonically trapped gas

353

reports the experimental results of Stewart et al. for the total contact based on the measurement of the momentum distribution at high momenta and on the large ω behaviour of the rf cross section (Schneider et al., 2009) Γ(ω) =

I 4π 2 ω 3/2

/m .

(18.46)

Stewart et al. (2010) have also tested the universal relations connecting the contact with the thermodynamic behaviour of a trapped Fermi gas. In particular, they have checked the validity of the sweep theorem and of the virial theorem, through the separate measurement of the release and oscillator energies. Figure 18.3 reports the experimental results for the contact (Hoinka et al., 2013) obtained from the large-k behaviour of the structure factor S(k) (see previous section), based on Bragg spectroscopic measurements at T ∼ 0. In both ﬁgures, the experimental data are compared with the theoretical predictions available along the crossover. The theoretical line in Figure 18.2 corresponds to the predictions of Werner et al. (2009), while the one in Figure 18.3 corresponds to quantum MC calculations carried out by the same authors combined with the LDA. Using eqn (18.41), which provides a useful relationship between the measured total contact and the local contact parameterized in terms of the dimensionless coeﬃcient α, Stewart et al. (2010) determined the value α ≈ 0.11, in fair agreement with the predictions of quantum Monte Carlo simulations. The local contact of the unitary Fermi gas was also measured at ﬁnite temperatures by Sagi et al. (2012), by selectively probing the centre of the trapped gas in rf spectroscopic experiments. At high temperatures these authors found good agreement with the predictions of Hu et al. (2011), based on the virial expansion.

19 Dynamics and Superﬂuidity of Fermi Gases Superﬂuidity is one of the most striking properties exhibited by ultracold Fermi gases, similar to superconductivity in charged Fermi systems. Interacting Fermi gases provide excellent opportunities to investigate superﬂuid phenomena. This is due to the large available values of the scattering length and to the possibility of exploring the whole BCS–BEC crossover. Among the most noticeable manifestations of superﬂuidity one should recall the absence of shear viscosity, the two-ﬂuid hydrodynamic nature of macroscopic dynamics, the irrotational quenching of the moment of inertia, and the existence of quantized vortices. The possibility of exploring these phenomena in ultracold gases is providing a unique opportunity for us to complement our present knowledge of superﬂuidity in neutral Fermi systems, previously limited to liquid 3 He, where pairing occurs in a p-wave state. In Section 19.1 we investigate the hydrodynamic behaviour exhibited by superﬂuids at zero temperature and its implications on the dynamics of uniform and trapped Fermi gases. In Section 19.2 we discuss the problem of the expansion of a Fermi gas, and in Section 19.3 we look at the Landau criterion for the critical velocity applied to a superﬂuid Fermi gas. In Section 19.4 we examine some consequences of superﬂuidity on the behaviour of the dynamic structure factor. In Section 19.5 we discuss the physical information that can be extracted on pairing phenomena, like the appearance of the gap in the superﬂuid phase, from the study of radiofrequency transitions. In Section 19.6 we apply Landau’s theory of twoﬂuid hydrodynamics to discuss superﬂuid phenomena at ﬁnite temperatures. Finally, in Section 19.7 we discuss the rotational properties of Fermi superﬂuids. There are other important manifestations of pairing phenomena in Fermi gases, like the behaviour of the pseudo-gap above the critical temperature, which are not discussed here. We refer to other review papers (see, for example, Zwerger (2012) for a discussion of these topics).

19.1

Hydrodynamics at zero temperature: sound and collective oscillations

A remarkable property of superﬂuids is that their macroscopic dynamic behaviour at zero temperature is governed by the equations of hydrodynamics. In contrast to normal ﬂuids at ﬁnite temperatures, where the hydrodynamic behaviour is ensured by

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

Hydrodynamics at zero temperature: sound and collective oscillations

355

collisions, in a superﬂuid it is the consequence of the occurrence of an order parameter, whose phase characterizes the superﬂuid velocity ﬁeld according to the law v=

∇S, 2m

(19.1)

where the factor 2 accounts for the fact that we are here considering a system of fermions where the relevant constituents which are responsible for the superﬂuid motion are pairs and the order parameter is associated with the oﬀ-diagonal long-range behaviour of the two-body density matrix. Equation (19.1) implies, in particular, the irrotationality of the superﬂuid motion; a feature with important consequences on the rotational behaviour. At zero temperature the hydrodynamic equations of superﬂuids consist of coupled and closed equations for the density and the velocity ﬁeld. Actually, in the absence of disorder or of modulated external potentials, the superﬂuid density coincides with the total density and the superﬂuid current coincides with the total current. The hydrodynamic picture assumes that the densities of the two spin components are equal and move in phase [n↑ (r, t) = n↓ (r, t) ≡ n(r, t)/2 and v↑ (r, t) = v↓ (r, t) ≡ v(r, t)] and that the current is hence given by j = nv. The hydrodynamic equations of T = 0 superﬂuids take the usual form ∂ n + ∇ · (nv) = 0, ∂t and ∂ m v+∇ ∂t

1 mv2 + μ(n) + Vho 2

(19.2) = 0,

(19.3)

already systematically employed to discuss the dynamics of Bose superﬂuids. Here μ(n) is the atomic chemical potential, ﬁxed by the equation of state of uniform matter. At equilibrium (v = 0) equation (19.3) reduces to the LDA equation (17.11) for the ground state density proﬁle at T = 0. Despite the quantum nature underlying the superﬂuid behaviour, the hydrodynamic equations have a classical form and do not depend explicitly on the Planck constant. This peculiarity raises the question whether the hydrodynamic behaviour of a cold gas can be used to probe the superﬂuid regime. In fact, as we will see, Fermi gases with resonantly enhanced interactions can easily enter a collisional regime above the critical temperature, where the dynamic behaviour describing an irrotational ﬂow is governed by the same equations (19.2) and (19.3). In this respect it is important to stress that collisional hydrodynamics admits the possibility of rotational components in the velocity ﬁeld which are strictly absent in the superﬂuid. A distinction between classical and superﬂuid hydrodynamics is consequently possible studying the rotational properties of the gas (Cozzini and Stringari, 2003b). Another possibility is provided by the study of the hydrodynamic behaviour at ﬁnite temperatures below the critical temperature where the hydrodynamic theory of superﬂuids describes the coupled motion of two ﬂuids associated with the normal and the superﬂuid components (see Section 19.6). It is also worth emphasizing that the hydrodynamic equations of

356

Dynamics and Superﬂuidity of Fermi Gases

superﬂuids have the same form both for Bose and Fermi systems, the eﬀects of statistics entering only the form of μ(n). The conditions of applicability can however be very diﬀerent in the two cases. The applicability of the hydrodynamic equations is in general limited to the study of macroscopic phenomena, characterized by long-wavelength excitations. In particular, the wavelengths should be larger than the healing length ξ. The value of ξ is easily estimated in the BEC limit where the Bogoliubov spectrum approaches the phonon dispersion law for wavelengths larger than ξ ∼ /mc. In the opposite BCS regime, the healing length is instead ﬁxed by the pairing gap. In fact, the Bogoliubov–Anderson phonon mode is deﬁned up to energies of the order ck ∼ Δgap , corresponding to ξ ∼ vF /Δgap . In both the BEC and BCS limits the healing length becomes increasingly large as kF |a| → 0. Near resonance the only characteristic length is ﬁxed by the average interatomic distance, and the hydrodynamic theory can be applied for all wavelengths larger than kF−1 . The hydrodynamic equations (19.2) and (19.3) can be linearized to describe the small oscillations with respect to equilibrium. Looking for small oscillations of the density, n(r, t) = n(r) + δn(r) exp(−iωt), where n(r) is the ground state density, the linearized equations take the form

∂μ 1 − ω 2 δn = ∇ · n∇ δn . (19.4) m ∂n In the absence of external conﬁnement the equilibrium density n0 is uniform and the solutions correspond to sound waves with dispersion ω = cq and mc2= n∂μ/∂n. In the BEC limit of the crossover one recovers the Bogoliubov result c = π2 add nd /m2 for the sound velocity, where add is the dimer–dimer scattering length and nd = n/2 is the molecular density. In the BCS limit one instead approaches √ √ the ideal gas value √ c = vF / 3. Finally, at unitarity one has the result c = ξB vF / 3 (see eqn (16.22)). The propagation of sound is aﬀected by the inhomogeneity of the medium. In a cylindrical conﬁguration (ωz = 0) the radial conﬁnement gives rise to a radial modulation of the density. For sound waves propagating with wavelengths larger than the radial size, the sound velocity can simply be calculated using the one-dimensional hydrodynamic result mc21D = n1D ∂μ1D /∂n1D , where n1D = dxdyn is the one-dimensional density and the one-dimensional chemical potential μ1D (n1D ) corresponds to the value of μ(n) calculated on the axis of the trap, where Vext = 0, as a function of n1D (see also Chapter 24). One ﬁnds (Capuzzi et al., 2006) ⎛ ⎜1 c1D = ⎜ ⎝m

⎞1/2

dxdyn dxdy(∂μ/∂n)

⎟ ⎟ ⎠ −1

,

(19.5)

where we have used the identity ∂n1D /∂μ1D = (∂n/∂μ)dxdy. Let us consider the case of radial harmonic conﬁnement. On the BEC side, where μ ∝ n, one recovers √ the result c1D = c/ 2, where c = n(∂μ/∂n)/m is the sound velocity calculated in uniform systems, with the value of the density calculated on the axis of the trap (see

Hydrodynamics at zero temperature: sound and collective oscillations

357

C0 / VF

0.5 0.4 0.3 0.2 –1

0

1

2 1/ kF a

3

4

5

6

Figure 19.1 Sound velocity in the centre of the trap measured along the BCS–BEC crossover (circles). The theory curves are obtained using eqn (19.5) and are based on diﬀerent equations of state: BCS mean-ﬁeld (dotted line), quantum Monte Carlo (solid line), and Thomas–Fermi molecular BEC with add = 0.60a (dashed line). The Fermi momentum kF corresponds to the value (17.9). From Joseph et al. (2007). Reprinted with permission from Physical Review c 2007, American Physical Society. Letters, 98, 170401;

also Section 12.2). At unitarity, where μ ∝ n2/3 , one instead ﬁnds c1D = 3/5c. The propagation of sound waves in interacting Fermi gases conﬁned by very elongated traps has been measured by Joseph et al. (2007) at very low temperatures. The experimental results are in good agreement with the estimate of c1D based on the QMC equation of state (see Figure 19.1). In the presence of three-dimensional harmonic trapping the lowest-frequency solutions of the hydrodynamic equations are discretized, their frequencies being of the order of the trapping frequencies. These modes correspond to wavelengths of the order of the size of the cloud. The classiﬁcation of the normal modes follows a procedure similar to the one employed in the case of Bose–Einstein condensed gases (see Chapter 12). Let us ﬁrst consider the case of isotropic trapping. At unitarity, by linearizing the hydrodynamic equations of motion, one ﬁnds the result 1/2 4 ω(nr , ) = ωho + nr (2 + + nr ) (19.6) 3 for the frequencies of the discretized oscillations. This result was ﬁrst obtained by Bruun and Clark (1999) and by Baranov and Petrov (2000) for a weakly interacting Fermi gas in the BCS regime where the equation of state has the same density dependence as at unitarity.√ The frequency of the monopole mode is equal to 2ωho , while in the Bose case it was 5ωho . The surface modes (nr = 0) have instead the same dependence on the quantum number as in the Bose case. They are in fact insensitive to the density dependence exhibited by the equation of state. Another interesting case is the one of axisymmetric trapping (ωx = ωy ≡ ω⊥ = ωz ), where the solutions can be classiﬁed in terms of the third component of angular

358

Dynamics and Superﬂuidity of Fermi Gases

momentum m. A general analytic solution of the hydrodynamic equations is again available for the surface modes with m = ±2, characterized by the divergency-free (∇·v = 0) velocity ﬁeld of the form v ∝ ∇(x ± iy)2 (or, equivalently, (∂μ/∂n)δn ∝ (x ± iy)2 ). The frequency √ of these surface modes, also called quadrupole oscillations, is given by ω(m = ±2) = 2ω⊥ . Another class of divergency-free oscillations, corresponding to m = ±1, is associated with the velocity ﬁeld v ∝ ∇z(x ± iy). In this case 2 + ω 2 . Like in BEC gases, the modes associated with the one ﬁnds ω(m = ±1) = ω⊥ z velocity ﬁelds ∇(xz) and ∇(yz), which correspond to linear combinations of the above m = ±1 modes, can be also regarded as a rigid rotation of the atomic cloud oscillating around the symmetry axis of the conﬁning trap. For this reason they are also called the scissors modes (see Section 14.3) and are easily excited through a sudden rotation of the symmetry axis of the trap. Both the frequencies of the m = ±2 and ±1 modes are insensitive to the equation of state and consequently coincide with the values predicted in Bose–Einstein condensates (see eqns (12.13) and (12.14)). They provide a useful criterion to characterize the occurrence of the hydrodynamic regime. For example, the frequency of the quadrupole m = ±2 mode diﬀers from the prediction 2ω⊥ of the collisionless regime characterizing the ideal gas model, revealing the importance of interactions accounted for by the hydrodynamic description. Both the quadrupole and the scissors modes have been the object of systematic experimental measurements in Fermi gases (see, for example, Altmeyer et al., 2007; Wright et al., 2007). These experiments reveal that, while at resonance and on the BEC side of the resonance the hydrodynamic regime is easily achieved in interacting Fermi gases, when one moves towards the BCS side the conditions for superﬂuidity are much more diﬃcult to attain, likely because of the low values of the critical temperature, and the behaviour of these modes approaches the collisionless regime. Unlike the divergency-free m = ±2 and m = ±1 modes discussed above, the m = 0 modes depend instead on the equation of state and have a compressional nature. Their frequency consequently varies along the BCS–BEC crossover and cannot be calculated in an analytic form except in some special cases. For example, at unitarity, where the equation of state at T = 0 has the power law dependence μ ∝ n2/3 on the density, the solutions of the linearized equations (19.2) and (19.3) are characterized by a velocity ﬁeld of the form v ∝ ∇[a(x2 + y 2 ) + bz 2 ] and their frequency is given by # 5 2 4 1 2 2 4 ω 2 (m = 0) = ω⊥ + ωz2 ± 16ωz4 − 32ω⊥ ωz + 25ω⊥ . (19.7) 3 3 3 In the isotropic limit (ω⊥ = ωz = ωho ) the frequencies approach the values ω = 2ωho √ and ω = 2ωho , corresponding to the monopole ( = 0, m = 0) and quadrupole ( = 2, m = 0) frequencies, respectively. In the limit of elongated traps (ωz ω⊥ ) the two solutions instead reduce to the radial (ω = 10/3ω⊥ ) and axial (ω = 12/5ωz ) breathing modes. It is worth noticing that these values diﬀer from the corresponding results holding for a Bose–Einstein condensate, due to the diﬀerent density dependence exhibited by the equation of state (see eqn (12.15)). Experimentally, both the radial and axial compression modes have been investigated (Kinast et al., 2004; Bartenstein et al., 2004b; Altmeyer et al., 2007) along the BCS–BEC crossover. In Figure 19.2 we show the experimental results of Altmeyer

Hydrodynamics at zero temperature: sound and collective oscillations

359

2.05

Normalized frequency

2.00

1.95

1.90

1.85

1.80 2.0

1.5

1.0 1/ kF a

0.5

0.0

Figure 19.2 Frequency of the radial compression mode for an elongated Fermi gas in units of the radial frequency. The curves refer to the equation of state based on the Bogoliubiov–de Gennes mean-ﬁeld theory (lower line) and Monte Carlo simulations (upper line). The Fermi momentum kF corresponds to the value (17.9). From Altmeyer et al. (2007). Reprinted with c 2007, American Physical Society. permission from Physical Review Letters, 98, 040401;

et al. (2007) for the radial breathing mode. At unitarity the agreement between theory and experiment is remarkably good. It is also worth noticing that the damping of the oscillation is smallest near unitarity. When we move from unitarity the collective oscillations exhibit other interesting features. Theory predicts that in the deep BEC regime the frequencies of both the axial and radial modes are higher than at unitarity. Furthermore, the ﬁrst corrections (also called Lee–Huang–Yang (LHY) correction) with respect to the mean-ﬁeld prediction can be calculated analytically, by accounting for the ﬁrst correction to the equation of state μd = gd nd produced by quantum ﬂuctuations. The resulting shifts (see Section 12.5) in the collective frequencies are positive and consequently, when one moves from the BEC regime towards unitarity, the dispersion law of the radial breathing mode in highly elongated traps exhibits a typical nonmonotonic behaviour, since it ﬁrst increases, due to the LHY eﬀect, and eventually decreases to reach the universal value 10/3ω⊥ at unitarity (Stringari, 2004). In general, the collective frequencies can be calculated numerically along the crossover by solving the hydrodynamic equations once the equation of state is known. Figure 19.2 also shows the predictions (Astrakharchik et al., 2005b) for the radial breathing mode in highly elongated traps, obtained using the equation of state of a diﬀusion Monte Carlo simulation and of the BdG mean-ﬁeld theory of Section 16.8. The Monte Carlo equation of state accounts for the LHY eﬀect, while the mean-ﬁeld

360

Dynamics and Superﬂuidity of Fermi Gases

theory misses it and provides a monotonic behaviour for the compressional frequency as one moves from the BEC regime to unitarity. The accurate measurements of the radial compression mode reported in the ﬁgure conﬁrm the Monte Carlo predictions and provide an important test of the equation of state of interacting Fermi gases at zero temperature. The behaviour of the breathing mode on the BCS side of the resonance exhibits diﬀerent features. Similarly to the case of the quadrupole mode, one expects that the system will soon lose superﬂuidity and eventually behave like a dilute collisionless gas whose collective frequencies are given by 2ω⊥ and 2ωz for the radial and axial modes, respectively. Experimentally, the transition was clearly observed in the radial mode (Kinast et al., 2004; Bartenstein et al., 2004b), where it occurs at about kF |a| ∼ 1. It is also associated with a strong increase of the damping of the collective oscillation. A case which deserves special attention is the breathing mode of the unitary gas for isotropic harmonic trapping. In this case an exact solution of the many-body problem is available (Castin, 2004) without invoking the hydrodynamic picture. One makes use of the following scaling ansatz for the normalized many-body wavefunction:

Ψ(r1 , . . . rN , t) = b−3N/2 ei(

j

˙ rj2 mb/2b−c)

Ψ0 (r1 /b, . . . rN /b),

(19.8)

where Ψ0 is the many-body wavefunction with energy E, b(t) is a time-dependent scaling variable and c(t) = E dt/b2 . Equation (19.8) satisﬁes the Bethe–Peierls boundary condition (9.18) if one works at unitarity where 1/a = 0. At the same time, for distances larger than the range of the force, where the Hamiltonian coincides with the kinetic energy, the Schr¨odinger equation is exactly satisﬁed by eqn (19.8), provided 2 ¨b = ωho − ω 2 b, ho b3

(19.9)

the initial equilibrium conﬁguration corresponding to...the value b = 1. This equation can be conveniently transformed into the equation B + 4ω02 B˙ = 0 with B ≡ b2 = r2 /r2 0 , where r 2 0 is the value of the square radius calculated with the wave function Ψ0 . The general solution of eqn (19.9) has the form B(t) = A sin(2ωho t+φ)+c with c2 = A2 + 1, the value of A ﬁxing the amplitude of the oscillation. One then ﬁnds that the square radius oscillates around the equilibrium value with the frequency ω = 2ωho , in agreement with the prediction of the hydrodynamic equations discussed above. Furthermore, the frequency of the oscillation is independent of its amplitude and the oscillation does not exhibit any damping. The same equation (19.9) also describes the breathing oscillation of two-dimensional Bose gases (see eqn (23.15)).

19.2

Expansion of a superﬂuid Fermi gas

In most experiments with ultracold atomic gases images are taken after expansion. These measurements provide information on the state of the gas in the trap and it is consequently of crucial importance to have an accurate theory describing the expansion. As discussed in Section 17.1, in the absence of interactions the expansion of a

Expansion of a superﬂuid Fermi gas

361

Fermi gas is asymptotically isotropic even if it is initially conﬁned by an anisotropic potential. Deviations from isotropy are consequently an important signature of the role of interactions. Hydrodynamic theory has been extensively used to analyse the expansion of Bose–Einstein condensed gases (see Section 12.7). The same theory has also been applied to investigate the expansion of an interacting Fermi gas at T = 0 (Menotti, Pedri, and Stringari, 2002). The hydrodynamic solutions are obtained starting from the equilibrium conﬁguration, corresponding to a Thomas–Fermi proﬁle, and then solving the equations (19.2) and (19.3) by setting Vho = 0 for t > 0. In general, the hydrodynamic equations should be solved numerically. However, at unitarity, where the equation of state has a power law dependence on the density, analytic solutions can be found, as in the case of a BEC gas, using a scaling ansatz x y z −1 n(x, y, z, t) = (bx by bz ) n , (19.10) , , bx by bz for the density, where n(x, y, z) is the ground state density. The scaling parameters bi obey the simple time-dependent equations: ¨bi −

ωi2 = 0. bi (bx by bz )2/3

(19.11)

The above equation is the fermionic analogue of the scaling law (12.42)–(12.43) introduced in Section 12.7 in the case of an expanding Bose gas. It is worth noticing that in the case of isotropic trapping this equation coincides with eqn (19.9), once the last term in (19.9), arising form the trapping potential, is set equal to zero. Diﬀerently from (19.9), eqn (19.11), which includes the case of anisotropic trapping, is valid only within the hydrodynamic approximation. From the solutions of eqn (19.11) one can calculate the aspect ratio as a function of time. For an axially symmetric trap (ωx = ωy ≡ ω⊥ ) this is deﬁned as the ratio between the radial and axial radii. In terms of the scaling parameters bi it can be written as b⊥ (t) ωz R⊥ (t) = . Z(t) bz (t) ω⊥

(19.12)

For an ideal gas the aspect ratio tends to unity, while the hydrodynamic equations yield an asymptotic value = 1. Furthermore, hydrodynamics predicts a peculiar inversion of shape during the expansion, caused by the hydrodynamic forces which are larger in the direction of larger density gradients. As a consequence, an initial cigar-shaped conﬁguration is brought into a disk shaped proﬁle at large times, and vice versa. One can easily estimate the typical time at which the inversion of shape takes place. For a highly elongated trap (ω⊥ ωz ) the axial radius is practically unchanged for short times, since the relevant expansion time along the z-axis is ﬁxed by 1/ωz . Conversely, the radial size increases rapidly and, for ω⊥ t 1 one expects R⊥ (t) ∼ R⊥ (0)ω⊥ t. One then ﬁnds that the aspect ratio is equal to unity when ωz t ∼ 1. In Figure 19.3 we show the predictions for the aspect ratio given by eqns (19.11) and (19.12) at unitarity, together with the experimental results of O’Hara et al. (2002)

362

Dynamics and Superﬂuidity of Fermi Gases

Aspect ratio [σx/σz]

2.5 2.0 1.5 1.0 0.5

0.0

0.5

1.0 1.5 Expansion time [ms]

2.0

Figure 19.3 Aspect ratio as a function of time measured during the expansion of an ultracold Fermi gas at unitarity (upper points) and for a noninteracting Fermi gas (lower points). The corresponding theoretical predictions, based respectively on hydrodynamic theory and ballistic expansion, compare well with experiments. From O’Hara et al. (2002). Reprinted by c 2002, AAAS. permission from Science, 298, 2179;

and the predictions of the ideal Fermi gas. The conﬁguration shown in the ﬁgure corresponds to an initial aspect ratio equal to R⊥ /Z = 0.035. The comparison strongly supports the hydrodynamic nature of the expansion of these ultracold Fermi gases. The experiment was repeated at higher temperatures and found to exhibit a similar hydrodynamic behaviour even at temperatures of the order of the Fermi temperature, where the system can not be superﬂuid. One then concludes that even in the normal phase the hydrodynamic regime can easily be reached as a consequence of collisions. This is especially plausible close to unitarity where the scattering length is very large and the free path of atoms is of the order of the interatomic distances. The anisotropic expansion exhibited by ultracold gases shares important analogies with the expansion observed in the quark gluon plasma produced in heavy ion collisions (see, for example, Kolb et al., 2001; Shuryak, 2004).

19.3

Phonon versus pair-breaking excitations and Landau’s critical velocity

In the previous section we described the discretized modes predicted by hydrodynamic theory in the presence of harmonic trapping. This theory describes correctly only the low-frequency oscillations of the system, corresponding to sound waves in a uniform body. When one considers higher excitation energies the dynamic response should also include dispersive corrections to the phononic branch and the breaking of pairs into two fermionic excitations.

Phonon versus pair-breaking excitations and Landau’s critical velocity

363

The interplay between phonon and pair-breaking excitations gives rise to diﬀerent scenarios along the crossover. In the BCS regime the threshold occurs at low frequencies and the phonon branch very soon reaches the continuum of single-particle excitations. The behaviour is quite diﬀerent in the opposite, BEC regime where the phonon branch extends up to high frequencies. At large momenta this branch actually loses its phononic character and approaches the dispersion 2 q 2 /4m, typical of a free molecule. In the deep BEC limit the phonon branch coincides with the Bogoliubov spectrum of a dilute gas of bosonic molecules. At unitarity the system is expected to exhibit an intermediate behaviour, the phonon branch surviving up to momenta of the order of the Fermi momentum. A detailed calculation of the excitation spectrum, based on a time-dependent formulation of the BdG mean-ﬁeld equations, was carried out by Combescot et al. (2006b). The results for the excitation spectrum provide a useful insight into the superﬂuid behaviour of the gas in terms of the Landau criterion, according to which a system can not give rise to energy dissipation if its velocity, with respect to a container or to a weakly interacting impurity at rest, is smaller than the Landau critical velocity deﬁned by the equation (see Section 6.1) ωq vc = min , (19.13) q q where ωq is the energy of an excitation carrying momentum q. According to this criterion the ideal Fermi gas is not superﬂuid because of the absence of a threshold for the single-particle excitations, which yields vc = 0. The interacting Fermi gas is instead superﬂuid, at T = 0, in all regimes. By inserting in (19.13) the single-particle dispersion law q of eqn (16.50), predicted by the approximate Bogoliubov–de Gennes mean-ﬁeld theory, one ﬁnds the result (19.14) m(vcpb )2 = Δ2 + μ2 − μ for the critical velocity associated with pair breaking. In the deep BCS limit kF |a| → 0, corresponding to Δ μ, eqn (19.14) approaches the exponentially small value vc = Δ/kF . On the BEC side of the crossover, however, the value (19.14) becomes increasingly large and the relevant excitations giving rise to Landau’s instability are no longer single-particle excitations but phonons and the critical velocity coincides with the sound velocity: vc = c. A simple estimate of the critical velocity along the whole crossover is then given by the expression vc = min c, vcpb . (19.15) Remarkably, one sees that vc has a maximum near unitarity (see Figure 19.4), further conﬁrming the robustness of superﬂuidity in this regime. The critical velocity has been measured by Miller et al. (2007) by moving a one-dimensional optical lattice at tunable velocity in a trapped gas (see Figure 19.5). Figure 19.6 shows the measured critical velocity along the BCS–BEC crossover, revealing a maximum near unitarity, as expected theoretically. An accurate theoretical prediction for the critical velocity

364

Dynamics and Superﬂuidity of Fermi Gases

Figure 19.4 Landau’s critical velocity (in units of the Fermi velocity) calculated along the crossover using BCS mean-ﬁeld theory. The ﬁgure clearly shows that the critical velocity is largest near unitarity. The dashed line is the sound velocity. From Combescot et al. (2006b).

Condensate number Nc [× 105]

5

4

3 v

2

1

0 0

2 4 6 Lattice velocity v [mm/s]

8

Figure 19.5 Onset of dissipation for superﬂuid fermions in a moving optical lattice. (inset) Schematic of the experiment in which two intersecting laser beams produced a moving optical lattice at the centre of an optically trapped cloud (trapping beams not shown). Number of fermion pairs which remained in the condensate Nc after being subjected to a V0 = 0.2 EF deep optical lattice for 500 ms, moving with velocity vL , at a magnetic ﬁeld of 822 G (1/kF a = 0.15). An abrupt onset of dissipation occurs at vc ∼ 6mm/s. From Miller et al. (2007). c 2007, American Reprinted with permission from Physical Review Letters, 99, 070402; Physical Society.

Dynamic structure factor Magnetic field [Gauss] 890 870 850 830 810 790 770

365

750

Critical velocity vc [mm/s]

6

5

4

–0.5

0.0 0.5 1.0 Interaction parameter 1/kF a

1.5

Figure 19.6 Measured critical velocity along the BCS–BEC crossover. The solid line is a guide to the eye. From Miller et al. (2007). Reprinted with permission from Physical Review c 2007, American Physical Society. Letters, 99, 070402;

should also include the possible excitation of vortex rings, whose role is known to be very important in the case of superﬂuid helium as well as the nonuniformity of the ﬂuid. A recent investigation of the critical velocity has focused on a pancake Fermi superﬂuid along the BEC-BCS crossover and has been implemented by rotating at diﬀerent velocities a focused laser beam of size of the order of the healing length (Weimer et al., 2015). Both the sound velocity and the critical velocity vc were measured in this experiment, and the value of vc turns out to be signiﬁcantly smaller than the value of the sound velocity. The observed reduction has been theoretically understood in the BEC regime in terms of the nonlinearity of the laser perturbation, ﬁnite temperature eﬀects, and the ﬁnite curvature of the rotating laser beam.

19.4

Dynamic structure factor

The dynamic structure factor provides an important characterization of many-body systems (see Section 7.1). In a Fermi superﬂuid, at low energy transfer, it gives information on the spectrum of collective oscillations, including the propagation of sound, while at higher energies it is sensitive to the behaviour of single-particle excitations and in particular to the pair-breaking mechanism. The dynamic structure factor is measured through inelastic scattering experiments in which the probe particle is weakly coupled to the many-body system so that the scattering may be described within the

366

Dynamics and Superﬂuidity of Fermi Gases

Born approximation. In dilute gases it can be accessed with stimulated light scattering by using two-photon Bragg spectroscopy (Stamper-Kurn et al., 1999), as extensively discussed in Section 12.8. The dynamic structure factor S(q, ω) is deﬁned by the general expression (7.31) and depends on the momentum q and energy ω transferred by the probe to the sample. It provides useful information on the excitation spectrum associated with the density operator ρˆq = j exp(−iq · rj ). Its deﬁnition is immediately generalized to other excitation operators like, for example, the spin density operator. The main features of the dynamic structure factor are best understood in uniform matter, where the excitations are classiﬁed in terms of their momentum. From the results of the previous sections one expects that, for suﬃciently small momenta, the dynamic structure factor relative to the density operator will be characterized by a sharp phonon peak and by a continuum of single-particle excitations above the threshold energy ωthr equal to 2Δgap as q → 0. The behaviour of the spin dynamic structure factor, relative to the spin density operator sˆq = j↑ exp(−iq·rj↑ )− j↓ exp(−iq·rj↓ ) is not instead sensitive to the phonon excitation and could consequently provide a more direct identiﬁcation of the gap. At higher momentum transfer the behaviour of the density dynamic structure factor depends crucially on the regime considered. In fact, for values of q of the order of the Fermi momentum the discretized phonon branch no longer survives on the BCS side of the resonance. At even higher momenta, corresponding to kF q 1/a, a regime achievable only on the BEC side of the resonance, the response is dominated by a sharp peak corresponding to the excitation of free molecules with energy 2 q 2 /4m (Combescot, Giorgini, and Stringari, 2006a). The molecular-like peak becomes less and less pronounced as one approaches the unitary point and disappears on the BCS side of the resonance where the response is expected to be similar to the one of an ideal Fermi gas. Experimental evidence for the excitation of the ‘molecular’ peak at energy ∼ 2 q 2 /4m has been reported by Hoinka et al. (2012) and Lingham et al. (2014). From the knowledge of the dynamic ∞ structure factor one can evaluate the static structure factor, given by N S(q) = 0 dωS(q, ω), a quantity directly related to the Fourier transform of the pair correlation function (see eqn (7.41)). For small values of q the density static structure factor of a uniform Fermi superﬂuid at T = 0 behaves like S(q) = q/(2mc) (see Section 7.4). The behaviour of the spin structure factor can instead be inferred from the inequality (7.64) with p = 0 yielding, for q → 0 where ωmin → 2Δgap , the result Sspin (q) ≤ q 2 /(4mΔgap ). The density structure factor of a superﬂuid Fermi gas has been measured by Hoinka et al. (2013) for large values of q, where the leading contribution to S(q) − 1 is ﬁxed by the contact parameter (see Section 18.5) and the static structure decreases for large q, as is clearly shown in Figure 18.1.

19.5

Radiofrequency transitions

As pointed out in Chapter 16, a challenging feature exhibited by Fermi superﬂuids is the occurrence of a gap in the single-particle excitation spectrum. In Section 19.3 we have shown that pair-breaking transitions characterize the excitation spectrum associated with the density–density response function and are directly visible in the

Radiofrequency transitions

367

dynamic structure factor. In principle, accurate measurements of the dynamic structure factor at small momentum transfer can give direct access to the threshold of pair-breaking transitions and hence to the value of Δgap . Information on pair-breaking eﬀects is also provided by transitions which outcouple atoms to a third internal state. Experiments using radiofrequency (rf) excitations were ﬁrst performed in a Fermi superﬂuid by Chin et al. (2004) in diﬀerent conditions of temperature and magnetic ﬁeld. The basic idea of these experiments is the same as for the measurement of the binding energy of free molecules. The structure of the rf transitions is determined by the Zeeman diagram of the hyperﬁne states in the presence of an external magnetic ﬁeld. Starting from a sample where two hyperﬁne states (hereafter called 1 and 2) are occupied, one considers single-particle transitions from state 2 (with energy E2 ) to a third, initially unoccupied, state 3 with energy E3 . The typical excitation operator characterizing these rf transitions has the form VRF = λ dr[ψˆ3† (r)ψˆ2 (r) + h.c.], where we have ignored the (small) momentum carried by the rf ﬁeld. The experimental signature of the transition is given by the appearance of atoms in state 3 or in the reduction of the number of atoms in state 2. In the absence of interatomic forces the transition is resonant at the frequency ω23 = (E3 − E2 )/. If instead the two atoms interact and form a molecule, the frequency required to induce the transition is higher since part of the energy carried by the radiation is needed to break the molecule. The threshold for the transition is given by the frequency ω = ω23 + |b |/, where |b | ∼ 2 /ma2 is the binding energy of the molecule (we are assuming here that no molecule is formed in the 1–3 channel). The actual dissociation line shape is determined by the overlap of the molecular state with the continuum and is aﬀected by the ﬁnal-state interaction between the atom occupying state 3 and the atom occupying state 1. In particular, the relationship between the value of the frequency where the signal is maximum and the threshold frequency depends on the value of the scattering length a31 characterizing the interaction between state 3 and state 1 (Chin and Julienne, 2005). For interacting many-body conﬁgurations along the BCS–BEC crossover a similar scenario takes place. In this case breaking pairs also costs energy so that the frequency shifts of the RF transitions provide information on the behaviour of the gap, although this information is less direct than in the case of free molecules. The ideal situation would take place if the interaction between the atoms in the ﬁnal state 3 and in the initial states 1 and 2 were negligible. The absorption of a photon then results in the transfer of an atom from the superﬂuid made of particles 1 and 2 to a ﬁnal state where we have a free atom in state 3 carrying momentum k while the system 1+2 (with one atom less in 2) occupies a many-body state with momentum −k (we can safely ignore the small momentum carried by the photon). Using the notation introduced in Section 16.7, the energy of the whole system, after the transition, will be Ef inal = Ek (N/2, N/2−1)+E3 +2 k 2 /2m = E(N/2, N/2)−μ+k +E3 +2 k 2 /2m, so that the threshold frequency is provided by the formula

δω ≡ (ω − ω23 ) = min[k + 2 k 2 /2m − μ], k

(19.16)

368

Dynamics and Superﬂuidity of Fermi Gases

where k is the quasi-particle excitation energy deﬁned in Section 16.8. In the BdG mean-ﬁeld theory k = Δ2 + (2 k 2 /2m − μ)2 (see (16.50)). Then minimization gives k = 0 and the threshold takes the simple form δω = Δ2 + μ2 − μ. Notice that the threshold does not correspond to the minimum of k which, in general, takes place at ﬁnite values of k. In the deep BEC limit of free molecules, where μ approaches the value −|b |/2 and Δ |μ|, the threshold (19.16) actually reproduces the result δω = |b |. In the opposite, BCS regime, where μ → EF , the single-particle gap Δgap is much smaller than the Fermi energy and one has instead δω = Δ2gap /2EF . Typical experimental results on 6 Li are shown in Figure 19.7, where the observed line shapes are presented for diﬀerent values of the temperature along the BCS–BEC crossover. In 6 Li the relevant scattering lengths a13 (< 0) and a12 are both large in modulus and ﬁnal-state interactions can not be ignored. On the BEC side of the resonance (lowest magnetic ﬁeld in Figure 19.7) one recognizes the emergence of the typical molecular line shape at low temperatures with the clear threshold eﬀect for the rf transition. In the most interesting region where kF |a| ∼ 1 many-body eﬀects become important and change the scenario of the rf transitions. While at high temperatures (upper row in Figure 19.7) the measured spectra still reveal the typical feature of the 0.5

720 G

822 G

837 G

875 G

a → ±∞

a = +120 nm

a = –600 nm

Fractional loss in |2

0.0 0.4 0.2 0.0 0.4 0.2 0.0 0

150

300 –15

0

15 30 –15 0 rf offset [kHz]

15 30

–15

0

15

30

Figure 19.7 rf spectra measured in 6 Li for various magnetic ﬁelds along the BCS–BEC crossover and for diﬀerent temperatures. The rf oﬀset δν = ν − ν23 is given relative to the atomic transition 2 → 3. The molecular limit is realized for B=720 G (ﬁrst column). The resonance regime is studied for B=822 G and 837 G (second and third columns). The data at 875 G (fourth column) correspond to the BCS side of the crossover. Upper row—signals of unpaired atoms at high temperatures (larger than TF ); middle row—signals for a mixture of unpaired and paired atoms at intermediate temperatures (fraction of TF ); lower row—signals for paired atoms at low temperatures (much smaller than TF ). From Chin et al. (2004). c 2004, AAAS. Reprinted by permission from Science, 305, 1128;

Radiofrequency transitions

369

(Δν/kHz)1/2

10

5

0 700

750

800 850 Magnetic field [G]

900

Figure 19.8 Frequency shift δνmax measured in 6 Li at low temperatures as a function of the magnetic ﬁeld for two diﬀerent conﬁgurations corresponding to TF = 1.2 μK (black triangles) and 3.6 μK (white triangles). The solid line shows the value δνmax predicted in the free molecular regime where it is essentially given by the molecular binding energy. From Chin c 2004, AAAS. et al. (2004). Reprinted by permission from Science, 305, 1128;

free atom transition, at lower temperatures the line shapes are modiﬁed by interactions in a nontrivial way. This is shown in Figure 19.8, where the shift δωmax = ωmax − ω23 , deﬁned in terms of the frequency ωmax where the rf signal is maximum, is reported for two diﬀerent values of TF . In the deep BEC regime the value of δωmax is independent of the density and is directly related to the binding energy of the molecule. In contrast, at unitarity and on the BCS side it shows a clear density dependence. The dependence on the density is even more dramatic in the BCS regime due to the exponential decrease of pairing eﬀects as kF |a| → 0. Since pairing eﬀects are density dependent and become increasingly weak as one approaches the border of the atomic cloud, one can not observe any gap in Figure 19.8 except on the BEC side of the resonance where the gap is density independent. Spatially resolved and three-dimensional reconstructed rf spectroscopy has now become available (Shin et al., 2007). This approach allows for a local identiﬁcation of the rf signal, thereby avoiding the problem of the density integration. Using this novel technique and choosing single-particle transitions which minimize the eﬀect of the ﬁnal state interaction, Schirotzek et al. (2008) were eventually able to extract the value of the pairing gap at unitarity (Δ = (0.44 ± 0.02)EF ), in remarkable agreement with the best Monte Carlo prediction Δ = (0.5 ± 0.03)EF at T = 0 (Carlson et al., 2003; Carlson and Reddy, 2005). A crucial improvement in the ﬁeld has been also provided by momentum-resolved rf spectroscopy (Stewart et al., 2008), obtained by directly measuring the energy and momenta of the outcoupled atoms. This approach allows, in principle, for the direct

370

Dynamics and Superﬂuidity of Fermi Gases

measurement of the spectral function (for a theoretical discussion see, for example, Haussman et al., 2009). A question is whether the energy gap persists above the critical temperature where pair correlations can be important even in the absence of oﬀ-diagonal long-range order and superﬂuidity. The problem is clearly formulated in the BEC regime, where molecules are formed at temperatures much higher than the critical temperature for their Bose–Einstein condensation, the typical transition temperature T ∗ for molecular dissociation being of the order of the binding energy and hence much larger than Tc as |b |/kB Tc ∼ 1/(kF a)2 1. On the BCS side, the formation of pairs and their condensation instead occur simultaneously (T ∗ ∼ Tc ). The behaviour of the spectral function along the crossover, and in particular at unitarity, has attracted signiﬁcant theoretical and experimental attention, in view also of the important analogies with the problem of the pseudo-gap in superconductors, and still remains a subject of great debate in the literature (see Randeria et al., 2012 and references therein).

19.6

Two-ﬂuid hydrodynamics: ﬁrst and second sound

The hydrodynamic theory developed in Section 11.1 describes eﬀectively the macroscopic behaviour of a superﬂuid Fermi gas at zero temperature. At ﬁnite temperatures the theory can be naturally generalized to include the dynamic description of the normal part. This gives rise to the hydrodynamic theory of two ﬂuids, whose equations were derived by Landau (1941) with special focus on liquid Helium (see Section 6.6). The equations of two-ﬂuid hydrodynamics consist, in addition to the equations of continuity ∂t ρ + ∇ · j = 0

(19.17)

and the equation for the superﬂuid velocity m∂t vs = −∇(μ + Vext ),

(19.18)

of the equation for the entropy density ∂t s + ∇ · (svn ) = 0

(19.19)

and for the current (Euler equation) ∂t j = −∇P − n∇Vext .

(19.20)

Equation (19.19), in particular, states that the entropy transport is provided by the normal component of the ﬂuid. In the above equations mj = ρs vs + ρn vn is the total current, given by the sum of the normal and superﬂuid contribution, and ρ = ρn + ρs is the total density. We have furthermore ignored nonlinear terms as well as dissipative eﬀects, which modify the equation for the entropy and for the current. The two-ﬂuid hydrodynamic equations are expected to hold if the collisional condition ωτ 1 is

Two-ﬂuid hydrodynamics: ﬁrst and second sound

371

ensured for the normal component of the gas, where τ is a typical collisional time accounting for thermal conductivity and viscosity eﬀects. General features of the twoﬂuid hydrodynamic equations have already been discussed in Section 6.6. In general, one expects solutions where the two ﬂuids move in phase (ﬁrst sound modes) and solutions where they move out of phase (second sound). Here we consider some speciﬁc applications of special interest for trapped Fermi gases. A major importance of these equations is due to the possibility of exploiting the role of the superﬂuid density, whose behaviour at ﬁnite temperatures is far from being understood in a strongly interacting Fermi gas. At T = 0 (where ρn = 0), the above equations reduce to the irrotational hydrodynamic equations discussed in Section 19.1. In fact, in this case the equation for the entropy identically vanishes, while the equation for the current coincides with the equation (19.18) for the superﬂuid velocity ﬁeld since, at thermal equilibrium, the Gibbs–Duhem thermodynamic equation dP = ndμ + sdT reduces to dP = ndμ. Above Tc , where the equation for the superﬂuid velocity ﬁeld disappears and ρs = 0, the other three equations coincide with the usual dissipationless equations of standard hydrodynamics. A ﬁrst useful application of the two-ﬂuid hydrodynamic equations in the presence of an axisymmetric harmonic potential concerns the derivation of exact analytic solutions at unitarity (Hou et al., 2013a) corresponding to the ansatz vs = vn ≡ v = ∇ β(t)(x2 + y 2 ) + δ(t)z 2 . This solution corresponds to the compressional m = 0 modes discussed in Section 19.1 at zero temperature. It is useful to show that this choice for the velocity ﬁeld is consistent with the scaling anstaz n(r, t) = e2α(t)+γ(t) n(r ), s(r, t) = e2α(t)+γ(t) s(r ) and T (t) = e(2α(t)+γ(t))2/3 T with r = (eα x, eα y, eγ z), where n(r), s(r) and T are the equilibrium values of the density, entropy density, and temperature. By inserting the above anstaz in the two-ﬂuid hydrodynamic equations, and taking into account the fact that the chemical potential, at unitarity, can be written as μ(T, n) = F (n)˜ μ(T /TF ) where μ ˜ is a dimensionless function, one can easily prove that the two ﬂuid hydrodynamic equations admit, in the linear limit of small oscillations, the same result (19.7), which holds for the m = 0 frequencies at zero temperature. With a similar procedure one can prove that the results for the surface modes with m = ± 2 and m = ± 1 also hold at ﬁnite temperatures. Actually, the results for the m = ± 2 and m = ± 1 surface modes are not restricted to unitarity, but are a general prediction of the hydrodynamic equations (19.17)–(19.20) applied to divergency-free modes (∇·v = 0) in the presence of harmonic trapping, holding for any form of the equation of state. The above discussion shows that, at unitarity, the collective frequencies of scaling nature have a temperature-independent frequency in the hydrodynamic regime and cannot consequently be employed to investigate the thermal eﬀect on the equation of state. This feature was conﬁrmed experimentally by Tey et al. (2013). In this work the consequences of the temperature dependence of the equation of state on the frequencies of the collective modes were actually investigated (both theoretically and experimentally) at unitarity looking at higher nodal compression modes where the above scaling considerations do not apply and the collective frequencies do actually exhibit a nontrivial temperature dependence.

372

Dynamics and Superﬂuidity of Fermi Gases

A major application of the two-ﬂuid hydrodynamic equations concerns the study of second sound and the role of the superﬂuid density. While some general discussions on the second sound solutions were discussed in Section 6.6 for uniform ﬂuids, here we discuss the propagation of sound in the presence of a tight radial trapping, a conﬁguration well suited to the current experimental possibilities. To this purpose we consider a gas in a highly elongated geometry, conﬁned radially by a tight harmonic potential with frequency ω⊥ . The eﬀect of the tight conﬁnement has the important consequence that the variations of the temperature δT (z, t) and of the chemical potential δμ(z, T ), as well as the axial velocity ﬁeld vnz (z, t), do not exhibit any dependence on the radial coordinate. The propagation of sound waves can then be considered one-dimensional in nature. The validity of this assumption is ensured by collisional eﬀects, which restore a radial local thermodynamic equilibrium and require the condition that the viscous penetration depth η/ρn1 ω is larger than the radial size of the system. Here ρn1 is the one-dimensional normal density, obtained by radial integration of the normal density, η is the shear viscosity, and ω is the frequency of the sound wave. In terms of the radial 2 trapping frequency ω⊥ the condition can be written in the form ω ω⊥ τ where τ is a typical collisional time, here assumed, for simplicity, to characterize both the eﬀects of viscosity and thermal conductivity. The condition of radial local thermodynamic equilibrium, which implies that the velocity ﬁeld of the normal component does not depend on the radial coordinates, would have a dramatic consequence in the presence of a tube geometry with hard walls. In fact, in this case the viscosity eﬀect near the wall would cause the vanishing of the normal velocity ﬁeld, with the consequent blocking of the normal ﬂuid. The resulting motion, involving only the superﬂuid with the normal component at rest, is called fourth sound, and was observed in liquid helium conﬁned in narrow capillaries. In the presence of radial harmonic trapping, this eﬀect is absent and the normal component can also propagate, allowing for the propagation of both ﬁrst and second sound. Under the above conditions of local radial equilibrium one can easily integrate radially the hydrodynamic equations (19.17)–(19.20) which then keep the same form as for the three-dimensional uniform gas (Bertaina et al., 2010): m∂t n1 + ∂z jz = 0

(19.21)

m∂t vsz = −∂z (μ1 (z) + Vext (z))

(19.22)

∂t s1 + ∂z (s1 vn ) = 0

(19.23)

(19.24) ∂t jz = −∂P1 − n∂z Vext (z), where n1 (z, t) = dxdyn(r, t), s1 (z, t) = dxdys(r, t), and P1 (z, t) = dxdyP (r, t) are the radial integrals of their three-dimensional counterparts, namely the particle density, the entropy density, and the local pressure, the integration accounting for the inhomogeneity caused by the radial component of the trapping potential. In the above equations jz = m(nn1 vnz + ns1 vsz ) is the current density, ns1 = dxdyns and nn1 = dxdynn are the superﬂuid and the normal one-dimensional densities, respectively, with n = nn1 + ns1 , while vsz and vnz are the corresponding velocity ﬁelds.

Two-ﬂuid hydrodynamics: ﬁrst and second sound

373

In eqn (19.22) μ1 (z, t) ≡ μ(r⊥ = 0, z, t) is the chemical potential calculated on the symmetry axis of the trapped gas. Its dependence on the one-dimensional density and on the temperature is determined by the knowledge of the radial proﬁle, which can be calculated employing the equation of state of uniform matter in the local density approximation. By setting the axial trapping Vext (z) equal to zero, which corresponds to considering a cylindrical geometry, we can look for sound wave solutions propagating with a phase factor of the form ei(qz−ωt) . One then derives the following equation for the sound velocity in this one-dimensional geometry:

c −c 4

2

1 m

∂P1 ∂n1

s¯1

1 ns1 T s¯21 ∂P1 1 ns1 T s¯21 + 2 + = 0, m nn1 c¯V 1 m nn1 c¯V 1 ∂n1 T

(19.25)

where s¯1 = s1 /n1 is the local one-dimensional entropy per particle and c¯V 1 = T (∂¯ s1 /∂T )n1 is the one-dimensional speciﬁc heat at constant volume. Equation (19.25) represents the one-dimensional counterpart of the most famous Landau equation (6.54) holding for uniform ﬂuids and yields two solutions, corresponding to the ﬁrst (c1 ) and second (c2 ) sound velocities. Simple results for the solutions of eqn (19.25) are obtained under the condition c22 c¯P 1 − c¯V 1 1, c21 c¯V 1

(19.26)

where c¯P 1 = T (∂ s¯1 /∂T )P1 is the one-dimensional speciﬁc heat at constant pressure. In this case one ﬁnds ∂P1 mc21 = (19.27) ∂n1 s¯1 for the ﬁrst sound velocity, corresponding to an adiabatic compression wave, and mc22 = T

ns1 s¯21 nn1 c¯P 1

(19.28)

for the second sound velocity. Notice that, under the condition (19.26), the ﬁrst sound velocity is independent of the superﬂuid density. In contrast the second sound velocity crucially depends on the superﬂuid density and consequently vanishes at the critical point. Some comments are in order here: (i) The assumption (19.26), yielding results (19.27) and (19.28), is well satisﬁed in strongly interacting superﬂuid Fermi gases in the whole temperature interval below Tc due to their small compressibility (from this point of view the behaviour of the solutions of the hydrodynamic equations deeply diﬀers from the case of dilute Bose gases discussed in Section 6.6). (ii) The expression (19.28) for the second sound velocity contains the speciﬁc heat at constant pressure. This reﬂects the fact that second sound actually corresponds to a wave propagating

374

Dynamics and Superﬂuidity of Fermi Gases

at constant pressure rather than at constant density. This diﬀerence is very important from the experimental point of view. In fact, even a small value of the compressibility is crucial in order to give rise to measurable density ﬂuctuations during the propagation of second sound (Sidorenkov et al., 2013). (iii) The thermodynamic ingredients P1 , s¯1 , c¯V 1 , and c¯P 1 are known with good precision at unitarity in a useful range of temperatures below the critical point. In fact, from the three-dimensional universal functions determined experimentally at unitarity (see Section 16.6), one can extract the relevant one-dimensional ingredients (Hou et al., 2013b). Figure 19.9 shows the propagation of ﬁrst and second sound measured in a highly elongated Fermi gas at unitarity. The excitation of ﬁrst and second sounds was obtained by generating, respectively, a sudden local perturbation of the density and of the temperature in the centre of the trapped gas. Due to the ﬁnite, although small, value of the thermal expansion coeﬃcient of the unitary Fermi gas the thermal perturbation, generating the second sound wave, also gives rise to a measurable density pulse. In this experiment, both the ﬁrst and second sound velocities were obtained by measuring, for a ﬁxed value of T , the time-dependence position of the density pulses generated by the perturbation. These measurements give access to the dependence of the sound velocity on the ratio T /TF1D , where TF1D

1 = kB

15π 8

2/5

(ω⊥ )

4/5

2 n21 2m

1/5 (19.29)

is a natural deﬁnition for Fermi temperature in one-dimensional cylindrically trapped conﬁgurations (Sidorenkov et al., 2013; Hou et al., 2013b). If n1 is calculated for an ideal Fermi gas at zero temperature, TF1D coincides with the usual three-dimensional deﬁnition TF = (2 /2mkB )(3π 2 n)2/3 of the Fermi temperature with n calculated on the symmetry axis. In the presence of axial trapping the value of T /TF1D actually increases as one moves from the centre, because of the density decrease, and eventually the density pulse reaches the transition point, where the superﬂuid vanishes. The ﬁgure actually shows that while the ﬁrst sound pulse propagates beyond the critical point and penetrates in the region where there is no superﬂuid (see dashed lines for the normal–superﬂuid boundary) the second sound pulse instead slows down when approaching the superﬂuid boundary without penetrating into the non-superﬂuid region. The corresponding values of the sound velocities are reported in Figure 19.10a. The dashed line in the upper part of the ﬁgure corresponds to the prediction (19.27) for the ﬁrst sound velocity which agrees remarkably well with the experimental results, showing that the temperature dependence of the ﬁrst sound velocity is now well understood. At zero temperature this value corresponds to c = ξB /5vF1D , # with vF1D = 2kB TF1D /m. In the lower part of the ﬁgure we show instead the measured values of the second sound velocity. These values have been employed to extract the value of the one-dimensional superﬂuid density, through eqn (19.28) (see Figure 19.10b). From these measurements it is possible to reconstruct the threedimensional superﬂuid density as a function of the ratio T /Tc , which is reported in Figure 16.4.

Two-ﬂuid hydrodynamics: ﬁrst and second sound

375

(a)

Time [ms]

(b) 20

+0.09 10

−0.06 0 (c)

Time [ms]

30

20 +0.06

10

−0.08 0

−400

0 Position [μm]

400

Figure 19.9 Observing the propagation of ﬁrst and second sound. (a) The basic geometry of exciting the optically trapped cloud with a weak, power-modulated repulsive laser beam, which perpendicularly intersects the trapping beam. The trapped cloud has a superﬂuid core, surrounded by a normal region. (b) and (c) Normalized diﬀerential axial density proﬁles δn1 (z, t)/n1, max taken for variable delay times after the excitation show the propagation of ﬁrst sound (local density increase, bright) and second sound (local decrease, dark). The temperature of the atomic cloud is T = 0.135(10)TFtrap . The vertical dashed lines indicate the axial region where superﬂuid is expected to exist according to a recent determination of the critical temperature (Ku et al., 2012). From Sidorenkov et al. (2013).

376

Dynamics and Superﬂuidity of Fermi Gases (a)

0.5 0.4

u/vF1D

0.3 0.2 0.1 0.0 (b) 0.6

ns1/n1

0.4

0.2

0.0

0.14

0.16

0.18

0.20

0.22

0.24

T/TF1D

Figure 19.10 First and second sound speeds and the superﬂuid fraction. (a) Speeds of ﬁrst and second sound, normalized to the local Fermi speed and plotted as a function of the reduced temperature. The data points and the solid lines refer to the data set of Figure 19.8. The shaded regions indicate the maximum range of variations from analysing diﬀerent data sets. The dashed line is a prediction for the ﬁrst sound velocity based on eqn (19.27) and the EOS from Hou et al. (2013b). The dotted horizontal line is the corresponding T = 0 value (16.22). Velocities are given in units of the one-dimensional Fermi velocity v1D = 2kB TF1D /m. (b) Temperature dependence of the one-dimensional superﬂuid fraction ns1 /n1 . In both panels, the grey shaded area indicates the uncertainty range of the superﬂuid phase transition according to Ku et al. (2012). From Sidorenkov et al. (2013).

19.7

Rotations and vortices

Superﬂuidity shows up in spectacular rotational properties. In fact, a superﬂuid cannot rotate like a rigid body, due to the irrotationality constraint (19.1) imposed by the existence of the order parameter. At low angular velocities an important macroscopic consequence of superﬂuidity is the quenching of the moment of inertia. At higher angular velocities the superﬂuid can instead carry angular momentum via

Rotations and vortices

377

the formation of vortex lines. The circulation around these vortex lines is quantized. When many vortex lines are created, a regular vortex lattice is formed and the angular momentum acquired by the system approaches the classical rigid-body value. By further increasing the angular velocity and approaching the radial trapping frequency, the centrifugal eﬀect becomes increasingly important and the system enters a new superﬂuid two-dimensional regime (lowest Landau level regime). Eventually, the rotating gas is expected to exhibit a phase transition to non-superﬂuid, quantum Hall conﬁgurations. Many of the features exhibited by rotating Fermi superﬂuids share important analogies with those of Bose–Einstein condensates (see Chapter 14), being the direct consequence of the irrotationality constraint imposed by superﬂuidity on the velocity ﬁeld. In this section we summarize some features exhibited by dilute Fermi gases in connection with the moment of inertia and the behaviour of the vortex lines. The moment of inertia Θ relative to the z-axis is deﬁned as the response of ˆ z according to Lz = L ˆ z = ΩΘ, where L ˆ z is the the system to a rotational ﬁeld −ΩL z-component of the angular momentum operator and the average is taken on the stationary conﬁguration in the presence of the perturbation. For a noninteracting gas trapped by a deformed harmonic potential, the moment of inertia can be calculated exactly. In the small-Ω limit (linear response) one ﬁnds the result Θ=

! mN (y 2 − x2 )(ωx2 + ωy2 ) + 2(ωy2 y 2 − ωx2 x2 ) 2 − ωy

ωx2

(19.30)

already discussed in Section 14.2, in the context of Bose gases (see eqn (14.16)). This result actually applies to both bosonic and fermionic ideal gases trapped by a harmonic potential. It assumes ωx = ωy , but admits a well-deﬁned limit when ωx → ωy . In the ideal Fermi gas, when the number of particles is large, one can use the Thomas–Fermi relationships x2 ∝ 1/ωx2 and y 2 ∝ 1/ωx2 for the radii. In this case the moment of inertia reduces to the rigid value of the moment of inertia: Θrig = N mx2 + y 2 .

(19.31)

For a noninteracting Bose–Einstein condensed gas at T = 0, where the radii scale according to x2 ∝ 1/ωx and y 2 ∝ 1/ωx , one instead ﬁnds that Θ → 0 as ωx → ωy . Interactions change the value of the moment of inertia of a Fermi gas in a profound way. To calculate Θ in the superﬂuid phase one can use the equations of two-ﬂuid hydrodynamics developed in the previous section, by considering a trap rotating with angular velocity Ω and looking for the stationary solution in the rotating frame. The ˆ z in equations of motion in the rotating frame are obtained by including the term −ΩL the Hamiltonian. For small values of Ω the new term in the Hamiltonian aﬀects only the equation of continuity for the density and the equation for the entropy density which take the form ∂t n + ∇ · (j − Ω × rn),

(19.32)

∂t s + ∇ · ((vn − Ω × r)nn ).

(19.33)

where j = nn vn + ns vs , and

378

Dynamics and Superﬂuidity of Fermi Gases

In the rotating frame the trap is described by the time-independent harmonic potential Vho and the hydrodynamic equations admit stationary solutions characterized by the irrotational velocity ﬁeld vs = −δΩ∇(xy),

(19.34)

where δ = (ωy2 − ωx2 )/(ωy2 + ωx2 ) is the deformation of the rotating potential, which coincides with the deformation of the atomic cloud if Ω is small. At equilibrium, the normal component of the velocity ﬁeld is instead given by vn = Ω × r,

(19.35)

and corresponds to a rigid ﬂow. In experiments, the rigid value of the rotation is induced by viscosity which drives the normal component into the rigid rotation (19.35). By evaluating the angular momentum Lz = m dr(r × v)n one then ﬁnds that the moment of inertia takes the form Lz Θ= = mδ 2 dxdy(x2 + y 2 )ns + m dxdy(x2 + y 2 )nn . (19.36) Ω At zero temperature, where the system is fully superﬂuid, the moment of inertia identically vanishes for axisymmetric conﬁgurations, pointing out the crucial role played by superﬂuidity, which makes the moment of inertia completely diﬀerent from the rigid value predicted by the noninteracting model. At ﬁnite temperatures, the moment of inertia is ﬁxed by the normal component and only above Tc does it coincide with the rigid value. First measurements of the moment of inertia of a Fermi superﬂuid gas at ﬁnite temperatures were reported by Riedl et al. (2011) at unitarity. The moment of inertia was measured by producing a sudden quadrupole deformation in the x–y plane and imaging its subsequent precession around the z-axis. Using the relationship (14.52) for the precession of the angle φ ﬁxing the axis of the quadrupole deformation in the x–y plane, Riedl et al. (2011) were able to extract the angular momentum of the rotating ﬂuid and observe the quenching of the moment of inertia due to superﬂuidity. The irrotational nature of the moment of inertia predicted at zero temperature by superﬂuid hydrodynamics has important consequences on the behaviour of the scissors mode. This is an oscillation of the system caused by the sudden rotation of a deformed # 2 trap which, in the superﬂuid case, has frequency ω = ωx + ωy2 and was discussed in Section 19.1. This result should be compared with the prediction of the normal gas in the collisionless regime where two modes with frequencies ω± = |ωx ± ωy | are found. The occurrence of the low-frequency mode |ωx − ωy | reﬂects the rigid value of the moment of inertia in the normal phase. The scissors mode, previously observed in a Bose–Einstein condensed gas (Marag` o et al., 2000), has also been investigated in ultracold Fermi gases (see Figure 19.11) along the BCS–BEC crossover (Wright et al., 2007). At unitarity and on the BEC side of the resonance one clearly observes the hydrodynamic oscillation, while when a becomes negative and small the beating between the frequencies ω± = |ωx ± ωy | reveals the transition to the normal collisionless regime. If the gas is normal but strongly collisional, as happens at unitarity above

Angle [º]

Rotations and vortices 30

30

20

20

10

10

0

379

0 0

2

4

6

8 0 Time [ms]

2

4

6

8

Figure 19.11 Time evolution of the angle characterizing the scissors mode in a Fermi gas at unitarity (left panel) and on the BCS side of the resonance (right panel). The measured frequencies agree well with the theoretical predictions (see text). From Wright et al. (2007).

the critical# temperature, classical hydrodynamics predicts an oscillation with the same frequency ωx2 + ωy2 . The persistence of the scissors frequency has been observed at unitarity by Wright et al. (2007), even above Tc . This result conﬁrms that near resonance the gas behaves hydrodynamically in a wide range of temperatures, below as well as above the critical temperature. One of the most important properties of superﬂuids, caused by the irrotationality condition for the velocity ﬁeld, concerns quantized vortices. Their existence was also conﬁrmed in ultracold Fermi gases along the BCS–BEC crossover (see Figure 19.12), providing undisputed evidence of the superﬂuidity of these systems. In these experiments, vortices are produced by spinning the atomic cloud with two laser beams and

792

0.7 BEC

Magnetic field [G] 833

0 Interaction parameter 1/kF a

852

–0.25 BCS

Figure 19.12 Experimental observation of quantized vortices in a superﬂuid Fermi gas along the BCS–BEC crossover. From Zwierlein et al. (2005b).

380

Dynamics and Superﬂuidity of Fermi Gases

are then observed by imaging the released cloud of molecules, which are stabilized through a rapid sweep of the scattering length to small and positive values during the ﬁrst millisecond of the expansion. This technique, which is similar to the one employed to measure the condensate fraction of pairs (see Section 16.9), increases the contrast of the vortex cores and therefore their visibility, thereby allowing for the observation of the vortex structure at unitarity as well as on the BCS of the resonance. A quantized vortex along the z-axis is associated with the appearance of a phase in the order parameter (16.41) in the form Δ(r) = Δ(r⊥ , z)eiφ ,

(19.37)

where φ is the azimuthal angle. A major diﬀerence with respect to vortices in Bose superﬂuids is that the velocity ﬁeld v = (/2m)∇φ depends on the mass of pairs in the denominator rather than on the mass of single atoms. This implies a diﬀerent quantization rule for the circulation of the vortex line π v·dl = (19.38) m and for the angular momentum carried by the vortex ˆ z = m dr(r × v)z n(r) = N , L 2

(19.39)

holding if the vortex line coincides with the symmetry axis of the density proﬁle. If the vortex is displaced towards the periphery of a trapped gas, the angular momentum takes a smaller value. The value of the circulation is instead independent of the position of the vortex and the radius of the contour. At higher angular velocities more vortices can be formed, giving rise to a regular vortex lattice (Abrikosov lattice, 1957). In this limit the angular momentum acquired by the system approaches the classical rigid-body value and the rotation is similar to that of a rigid body, characterized by the law ∇ × v = 2Ω. Using result (19.38) ˆ, and averaging the vorticity over several vortex lines one ﬁnds ∇ × v = (π/m)nv z where nv is the number of vortices per unit area. It then follows that the density of vortices nv (number of vortices per unit area) is related to the angular velocity Ω by the relation nv =

2m Ω, π

(19.40)

√ showing, in particular, that the distance between vortices (proportional to 1/ nv ) depends on the angular velocity but not on the density of the gas. By measuring the number of vortices and the size of the cloud and using eqn (19.40), Zwierlein et al. (2005) were actually able to check that the value of the stirring frequency employed in their experiments is consistent with the quantum of circulation h/2m, excluding the value h/m predicted for a bosonic superﬂuid. It is also worth noting that, due to the repulsive quantum pressure eﬀect characterizing Fermi gases, one can

Rotations and vortices

381

realize trapped conﬁgurations with a large size R⊥ hosting a large number of vortices 2 Nv = πR⊥ nv , even with relatively small values of Ω. For example, choosing Ω = ω⊥ /3, ωz ω⊥ and N = 106 , one predicts Nv ∼ 130 at unitarity, which is signiﬁcantly larger than the number of vortices that one can produce in a dilute Bose gas with the same angular velocity. Similarly to the Bose case at large angular velocities the vortex lattice is responsible for a bulge eﬀect associated with the increase of the radial size of the cloud and consequently with a modiﬁcation of the aspect ratio. In fact, in the presence of an average rigid rotation, the eﬀective potential felt by the atoms is given by Vho − 2 (m/2)Ω2 r⊥ and the new Thomas–Fermi radii satisfy the relationship 2 − Ω2 Rz2 ω⊥ = , 2 R⊥ ωz2

(19.41)

showing that at equilibrium the angular velocity can not overcome the radial trapping frequency. This formula can be used to determine directly the value of Ω by just measuring the in situ aspect ratio of the atomic cloud. A challenging problem concerns the visibility of the vortex lines. As we have already pointed out, due to the smallness of the healing length, especially at unitarity, they can not be observed in situ, but only after expansion. Furthermore the contrast in the density is reduced with respect to the case of Bose–Einstein condensed gases. Actually, while the order parameter vanishes on the vortex line the density does not, unless one works in the deep BEC regime. In the opposite BCS regime the order parameter is exponentially small and the density proﬁle is practically unaﬀected by the presence of the vortex. The explicit behaviour of the density near the vortex line requires the implementation of a microscopic calculation. This can be carried out along the lines of the mean-ﬁeld theory developed in Section 16.8. While this approach is approximate, it nevertheless provides a useful, consistent description of the vortical structure along the whole crossover. The vortex is described by the solution of the Bogoliubov–de Gennes equation (16.48), corresponding to the ansatz √ ui (r) = un (r⊥ )e−imφ eikz z / 2πL √ (19.42) vi (r) = vn (r⊥ )e−i(m+1)φ eikz z / 2πL, for the normalized functions ui and vi , where (n, m, kz ) are the usual quantum numbers of cylindrical symmetry and L is the length of the box in the z-direction. The ansatz (19.42) is consistent with the dependence (19.37) of the order parameter Δ on the phase φ. Calculations of the vortex structure based on the above approach have been carried out by several authors (see, for example, Nygaard et al., 2003; Sensarma et al., 2006). An important feature emerging from these calculations is that, near the vortex line, the density contrast is reduced at unitarity with respect to the BEC limit. It is ﬁnally worth observing that the achievement of the centrifugal limit for a superﬂuid containing a vortex lattice can not be ensured on the BCS side of the resonance. In fact, due to the bulge eﬀect (19.41), the centrifugal limit is associated

382

Dynamics and Superﬂuidity of Fermi Gases

with a strong decrease of the density and hence, for a < 0, with an exponential decrease of the order parameter Δ. It follows that the superﬂuid cannot support rotations with values of Ω too close to ω⊥ and that the system will exhibit a transition to the normal phase (Zhai and Ho, 2006; Veillette et al., 2006). If Ω becomes too close to ω⊥ , superﬂuidity will eventually also be lost at resonance and on the BEC side of the resonance because the system enters the quantum Hall regime (see Section 23.3).

20 Spin-polarized Fermi Gases The description of Fermi superﬂuidity presented in the previous sections was based on the assumption that the gas has an equal number of atoms occupying two diﬀerent spin states. One can also consider more complex conﬁgurations of spin imbalance where the number of atoms in the two spin states is diﬀerent (N↑ = N↓ ) as well as mixtures of atomic species with diﬀerent masses (m↑ = m↓ ), including Fermi–Fermi and Bose–Fermi mixtures. This chapter is mainly devoted to the discussion of the magnetic properties of the repulsive Fermi gas (Section 20.1), the competition between superﬂuidity and spin polarization (Sections 20.2–20.4) and the problem of the Fermi polaron (Section 20.5).

20.1

Magnetic properties of the weakly repulsive Fermi gas

In Section 16.3 we discussed the behaviour of a weakly repulsive Fermi gas. In the presence of a Feshbach resonance the resulting conﬁguration corresponds to a metastable branch with positive values of the scattering length. Experimentally, it can be produced by switching the scattering length on adiabatically starting from a noninteracting conﬁguration (a = 0). This branch is metastable since a more stable conﬁguration corresponds to the formation of dimers, resulting, at low temperatures, in a Bose– Einstein condensed phase, corresponding to the BEC limit of the BCS–BEC crossover discussed in Chapter 16. An interesting question concerns the magnetic properties of the repulsive branch. In fact, systems interacting with a suﬃciently strong repulsive force are expected to undergo a phase transition to a ferromagnetic phase (itinerant ferromagnetism). First experimental attempts to realize such a phase were reported by Jo et al. (2009). The emergence of the phase transition is associated with the occurrence of the socalled Stoner instability (Stoner, 1933), initially introduced to describe itinerant ferromagnetism in an electron gas with screened Coulomb interaction (see, for example, Snoke, 2008). A simple model which captures the qualitative features of the expected phase transition is provided by the expression E = Ekin + Eint , with Ekin = (3/5)N↑ EF↑ + (3/5)N↓ EF↓ and Eint = gN↑ N↓ /V with g = 4π2 a/m. In terms of the magnetization η = (n↑ − n↓ )/n of the gas, where n↑,↓ = (n/2)(1 ± η) are the densities of the two

Bose–Einstein Condensation and Superfluidity. Lev Pitaevskii and Sandro Stringari. c Lev Pitaevskii and Sandro Stringari 2016. Published 2016 by Oxford University Press.

384

Spin-polarized Fermi Gases

spin components and n = n↑ + n↓ is the total density, the energy per particle of the interacting conﬁguration takes the simple form

E 3 1 1 10 5/3 5/3 = EF (1 + η) + (1 − η) + kF a(1 + η)(1 − η) , (20.1) N 5 2 2 9π which reduces to the ﬁrst two terms of the expansion (16.8) in the absence of magnetization (η = 0). In this simple model the lowest energy conﬁguration is the result of the competition between the repulsive term which favours magnetization, and the kinetic energy which instead favours equal population of the two spin states. If the repulsive term kF a is too large the system undergoes phase separation characterized by the formation of spin domains (itinerant ferromagnetism). The corresponding (secondorder) phase transition takes place when the second derivative of E with respect to the magnetization becomes negative, corresponding to the onset of a negative value of the magnetic susceptibility. Using eqn (20.1) it can immediately be found that the instability takes place for kF ac = π/2 ∼ 1.57. For smaller values of kF a the energy (20.1) exhibits a minimum at η = 0. For larger values of kF a the value η = 0 instead corresponds to a local maximum and the system exhibits spontaneous magnetization. One should, however, point out that the mean-ﬁeld description (20.1) is expected to be accurate only for small values of the interaction parameter kF a and consequently this theory can provide only a rough estimate of the ferromagnetic phase transition. A better insight into the problem is obtained by evaluating the inverse magnetic susceptibility χ of the repulsive Fermi gas up to quadratic terms in the scattering length a, taking into account beyond-mean-ﬁeld corrections, in analogy with the second-order expansion (16.5) of the energy in terms of the scattering length. The result is (see, for example, Recati and Stringari, 2011) χ0 2 16(2 + ln 2) = 1 − kF a − (kF a)2 , χ π 15π 2

(20.2)

where χ0 = 3n/2EF is the susceptibility of the ideal Fermi gas. If extrapolated to the critical point where χ−1 = 0, the second-order expansion (20.2) gives a smaller critical value kF ac ∼ 1.05. Quantum Monte Carlo simulations (Pilati et al., 2010; Chang et al., 2011), applied to a Fermi gas interacting with repulsive forces, predict the ferromagnetic phase transition for even smaller critical values (kF ac ∼ 0.8). The precise determination of the critical value of kF a actually depends on the explicit model assumption for the interatomic potential, as the thermodynamic properties of the system cannot be expressed in a universal form as a function of the parameter kF a unless one limits the analysis to the small-a expansion (20.2). The nature of the phase transition, including second-order eﬀects in the scattering length, was investigated by Duine and MacDonald (2005) who concluded that the transition is of ﬁrst-order nature, diﬀerent from the prediction of mean-ﬁeld theory. In the presence of a Feshbach resonance the fate of the system for large values of kF a is dominated by collisional eﬀects, which bring the system into the energetically

Superﬂuidity and magnetization

385

more favourable molecular conﬁguration belonging to the superﬂuid branch of the BCS–BEC crossover. Through a careful analysis of the spin ﬂuctuations exhibited by the repulsive Fermi gas for large values of the scattering length, Sanner et al. (2012) have actually shown that the instability observed in the experiment of Jo et al. (2009) is not due to the onset of itinerant ferromagnetism and that the system exhibits a transition to the more stable molecular conﬁguration of dimers (see Section 16.4) before reaching the ferromagnetic instability. More promising perspectives to observe the Stoner instability are provided by ﬁnitetemperature conﬁgurations. He et al. (2014) have predicted that the unitary Fermi gas undergoes the ferromagnetic transition at above 1.5TF , above which the decay rate into pair formation becomes vanishingly small.

20.2

Superﬂuidity and magnetization

The problem of spin imbalance has a long history in the context of BCS theory of superconductivity. In superconductors, due to the fast relaxation between diﬀerent spin states leading to balanced spin populations, the only possibility for creating the asymmetry is to add an external magnetic ﬁeld. However, in bulk superconductors this ﬁeld is screened by the orbital motion of electrons (Meissner eﬀect). The situation in superﬂuid Fermi gases is more favourable. In fact, in this case, the relaxation time is very long and the numbers of atoms occupying diﬀerent spin states can be considered as independent variables. Let us recall that the mechanism of BCS superﬂuidity, in the regime of small and negative scattering lengths, arises from the pairing of particles of diﬀerent spinoccupying states with opposite momenta, close to the Fermi surface. This mechanism is inhibited by the presence of spin imbalance, since the Fermi surfaces of the two components do not coincide and pairs with zero total momentum are diﬃcult to form. Eventually, if the gap between the two Fermi surfaces is too large, superﬂuidity is broken and the system undergoes a quantum phase transition towards a normal state. The existence of a critical value for the polarization is easily understood by noticing that, at zero temperature, the unpolarized gas is superﬂuid, while a fully polarized gas is normal due to the absence of interactions. The occurrence of such a transition was ﬁrst suggested by Clogston (1962) and Chandrasekhar (1962) who predicted the occurrence of a ﬁrst-order transition from the normal to the superﬂuid state. This transition takes place when the gain in the grand-canonical energy E(N↑ , N↓ )−μ↑ N↑ − μ↓ N↓ associated with the ﬁnite polarization of the normal phase is equal to the energy diﬀerence between the normal and the superﬂuid unpolarized states. In the BCS regime one ﬁnds the critical condition h≡

μ↑ − μ↓ Δgap = √ , 2 2

(20.3)

where we have used expression (16.20) for the ground state energy in the superﬂuid phase and Δgap = (2/e)7/3 EF eπ/2kF a is the BCS gap. We have also assumed the spindown particles to be the minority component. The chemical potential diﬀerence h

386

Spin-polarized Fermi Gases

in the above equation plays the role of an eﬀective magnetic ﬁeld. In terms of the polarization P =

N↑ − N↓ , N↑ + N↓

(20.4)

it can be expressed through the relationship h = 2EF P/3, which holds if P 1. The condition (20.3) then immediately yields the critical value of P at which the system phase separates: 3 Pc = √ 8

7/3 2 e−π/2kF |a| . e

(20.5)

For P > Pc the system is normal and corresponds to a uniform mixture of the two spin components. For P < Pc the system is instead in a mixed state, where the unpolarized BCS superﬂuid coexists with the normal phase which accommodates the excess polarization. In this mixed state, the chemical potential diﬀerence of the normal phase retains the critical value (20.3) irrespective of polarization, a decrease in P being accounted for by an increase in the volume fraction of the superﬂuid phase which eventually occupies the entire volume for P = 0. An important remark concerning the Clogston–Chandrasekhar condition (20.3) is that the critical eﬀective magnetic ﬁeld h is smaller than the superﬂuid gap Δgap . If one had h > Δgap the above scenario would not apply because the system would prefer to accommodate the excess polarization by breaking pairs and creating quasi-particles. The gapless superﬂuid realized in this way would be homogeneous and the transition to the normal state would be continuous. Such a uniform phase is indeed expected to occur in the deep BEC regime. The physical understanding of polarized Fermi gases became more complicated when exotic superﬂuid phases were proposed, such as the inhomogeneous superﬂuid Fulde–Ferrell–Larkin–Ovchinnikov (FFLO) state (Fulde and Ferrell, 1964; Larkin and Ovchinnikov, 1964). In the FFLO state the superﬂuid exhibits a spontaneous breaking of translational symmetry with a periodic structure of the order parameter of the form Δ(x) ∝ cos(qx), where the direction of the x-axis is arbitrary (Fulde and Ferrell actually predicted the occurrence of an order parameter of the form exp(iqx) causing the appearance of a current in the ground state wave function). The wave vector q is proportional to the diﬀerence of the two Fermi wave vectors q ∝ kF ↑ − kF ↓ with a proportionality coeﬃcient of order unity. The excess spin-up atoms are concentrated near the zeros of the order parameter Δ(x). One can show that in the BCS limit the FFLO phase exists for h < 0.754Δgap , corresponding to the tiny interval of polarization 0 < P < 1.13Δgap /EF , while for P > 1.13Δgap /EF the system is normal (see, for example, Takada and Izuyama, 1969). In the deep BCS regime this scenario is more energetically favourable compared to the Clogston–Chandrasekhar transition which would take place at Pc = 1.06Δgap /EF . The FFLO state is of interest both in condensed matter physics and in elementary particle physics, even though direct experimental evidence of this phase is still lacking (for reviews, see Casalbuoni and Nardulli (2004) and Combescot (2007)).

Phase separation at unitarity

387

In ultracold gases the BCS regime is not easily achieved due to the smallness of the gap parameter and one is naturally led to explore conﬁgurations with larger values of kF |a|, where the concept of Fermi surface loses its meaning due to the broadening produced by pairing. A major question is whether the FFLO phase survives when correlations are stronger and if it can be realized in trapped conﬁgurations. Its existence at unitarity is still a debated question (for a recent review see Zwerger, 2012). An important region of the phase diagram is also the deep BEC regime of small and positive scattering lengths, where the energetically favourable phase consists of a uniform mixture of a superﬂuid gas of bosonic dimers and of a normal gas of spin-polarized fermions. The general problem of an interacting mixture of bosons and fermions was investigated by Viverit, Pethick, and Smith (2000) who derived the conditions of miscibility in terms of the values of the densities and masses of the two components and of the boson–boson and boson–fermion scattering lengths (see Section 21.5).

20.3

Phase separation at unitarity

A possible scenario for the equation of state of spin-imbalanced conﬁgurations at unitarity is based on the phase separation between an unpolarized superﬂuid and a polarized normal gas similar to the Clogston–Chandrasekhar transition discussed in the previous section (De Silva and Mueller, 2006a; Haque and Stoof 2006; Chevy, 2006a). An important ingredient of this scenario, not accounted for by the mean-ﬁeld description, is the proper inclusion of interaction eﬀects in the normal phase (Chevy 2006b; Lobo et al., 2006; Bulgac and Forbes, 2007). While there is not at present a formal proof that the phase-separated state is the most energetically favourable, the resulting predictions agree well with the experimental ﬁndings (see next section). The unpolarized superﬂuid phase was described in detail in Section 16.6 and is characterized, at unitarity, by the T = 0 equation of state ES 3 = ξB EF , N 5

(20.6)

where ES is the energy of the system, N is the total number of atoms, ξB is the Bertsch parameter, and EF = (2 /2m)(3π 2 nS )2/3 is the Fermi energy with nS = 2n↑ = 2n↓ the total density of the gas. Starting from (20.6) one can derive the pressure PS = −∂E/∂V and the chemical potential μS = ∂ES /∂N . In contrast to the superﬂuid, the normal phase is polarized and consequently its equation of state will also depend on the concentration x = n↓ /n↑ ,

(20.7)

which, in the following, will be assumed to be smaller or equal to 1, corresponding to N↑ ≥ N↓ . A convenient way to build the x-dependence of the equation of state is to take the point of view of a dilute mixture where a few spin-down atoms are added to a non-interacting gas of spin-up particles. When x 1, the energy of the system can be written in the form (Lobo et al., 2006) EN (n↑ , x) m 3 = EF ↑ 1 − Ax + ∗ x5/3 + . . . , (20.8) N↑ 5 m

388

Spin-polarized Fermi Gases

where EF ↑ = (2 /2m)(6π 2 n↑ )2/3 is the Fermi energy of the spin-up particles. The ﬁrst term in eqn (20.8) corresponds to the energy per particle of the noninteracting gas, while the term linear in x gives the binding energy of the spin-down particles. Equation (20.8) assumes that, when we add spin-down particles creating a small ﬁnite density n↓ , they form a Fermi gas of quasi-particles with eﬀective mass m∗ occupying, at zero temperature, all the states with wave vector k up to kF↓ = (6π 2 n↓ )1/3 and contributing to the total energy (20.8) with the quantum pressure term proportional to x5/3 . The interaction between the spin-down and spin-up particles is accounted for by the dimensionless parameters A and m/m∗ . The expansion (20.8) should in principle include additional terms originating from the interaction between quasi-particles and exhibiting a higher-order dependence on x. The values of the coeﬃcients entering (20.8) can be calculated using ﬁxed-node diﬀusion Monte Carlo simulations where one spin-down atom is added to a noninteracting Fermi gas of spin-up particles. The results of these calculations are A = 0.97(2) and m∗ /m = 1.04(3) (Lobo et al., 2006). The same value of A has been obtained from a diagrammatic Monte Carlo calculation (Prokof’ev and Svistunov, 2007) and also employing a simple variational approach based on a single particle-hole wave function (Chevy, 2006b; Combescot et al., 2007). These latter approaches provide a larger value of the eﬀective mass (m∗ /m ∼ 1.2). The prediction of eqn (20.8) for the equation of state is reported in Figure 20.1, where we also show the FN-DMC results obtained for 1.15 1.10

E/N (3EF /5)

1.05 1.00 0.95 0.90 Xc = 0.44

0.85 0.80 0.0

0.2

0.4

0.6

0.8

1.0

X

Figure 20.1 Equation of state of a normal Fermi gas as a function of the concentration x. The solid line is a polynomial best ﬁt to the QMC results (circles). The dashed line corresponds to the expansion (20.8). The dot–dash line is the coexistence line between the normal and the unpolarized superﬂuid states, and the arrow indicates the critical concentration xc above which the system phase separates. For x = 1, both the energy of the normal and of the superﬂuid (diamond) states are shown. From Giorgini et al. (2008).

Phase separation at unitarity

389

ﬁnite values of the concentration x. It is remarkable to see that the expansion (20.8) reproduces quite well the best ﬁt to the FN-DMC results, up to the large values of x where the transition to the superﬂuid phase takes place. In particular, the repulsive term in x5/3 , associated with the Fermi quantum pressure of the minority species, plays a crucial role in determining the x-dependence of the equation of state. Notice that when x = 1 (N↑ = N↓ = N/2) the energy per particle in the normal phase is smaller than the ideal gas value 3EF ↑ /5, reﬂecting the attractive nature of the force, but larger than the value in the superﬂuid phase (0.42)3EF ↑ /5 predicted by the same Monte Carlo algorithm. We can now determine the conditions of equilibrium between the normal and the superﬂuid phase. A ﬁrst condition is obtained by imposing that the pressures of the two phases are equal: ∂ES ∂EN = , ∂VS ∂VN

(20.9)

where VS and VN are the volumes occupied by the two phases, respectively. A second condition is obtained by requiring that the chemical potential of each pair of spinup–spin-down particles is the same in the two phases. In order to exploit this latter condition one takes advantage of the thermodynamic identity μS = (μ↑ + μ↓ )/2 for the chemical potential in the superﬂuid phase, yielding the additional relation ∂ES 1 ∂EN ∂EN = , (20.10) + ∂N 2 ∂N↑ ∂N↓ where we have used the expression μ↑(↓) = ∂EN /∂N↑(↓) for the chemical potentials of the spin-up and spin-down particles calculated in the normal phase. Equation (20.10), combined with (20.9), permits us to determine the critical values of the thermodynamic parameters characterizing the equilibrium between the two phases. For example, if applied to the BCS regime where EN = 3/5(N↑ EF ↑ + N↓ EF ↓ ) and ES = EN − 3N Δ2gap /8EF (see eqn (16.20)), this approach reproduces the Clogston– Chandrasekhar condition (20.5) (Bedaque, Caldas, and Rupak, 2003). In contrast, at unitarity, a calculation based on the QMC values of EN and ES yields the values xc = 0.44, corresponding to Pc = (1 − xc )/(1 + xc ) = 0.39, and (nN /nS )c = 0.73, where nN = n↑ + n↓ is the density of the normal phase in equilibrium with the superﬂuid (Lobo et al., 2006). For values of the polarization larger than Pc = 0.39 the stable conﬁguration is the uniform normal phase, while if we increase the number of the spin-down particles (corresponding to a reduction of P ) there will be a phase separation between a normal phase with the concentration xc = 0.44 and a superﬂuid unpolarized phase. The phase transition has ﬁrst-order character, consistent with the critical value h = 0.81Δgap being smaller than the superﬂuid gap. In particular, while the spin-up density is practically continuous, the density of the spin-down particles exhibits a signiﬁcant jump at the transition. Let us ﬁnally point out that the parameters characterizing the transition between the superﬂuid and the normal phases depend in a crucial way on the many-body scheme employed for the calculation. For example, if instead of the Monte Carlo results we use the BCS mean-ﬁeld theory of Section 16.8

390

Spin-polarized Fermi Gases

and the noninteracting expression EN = 3/5(N↑ EF ↑ + N↓ EF ↓ ) for the energy of the normal phase, we ﬁnd the very diﬀerent value xc = 0.04 for the critical concentration.

20.4

Phase separation in harmonic traps at unitarity

The results presented in the previous section can be used to calculate the density proﬁles in the presence of harmonic trapping. We make use of the local density approximation, which permits us to express the local value of the chemical potential of each spin species as μ↑(↓) (r) = μ0↑(↓) − Vho (r),

(20.11)

the values of μ0↑(↓) being ﬁxed by the proper normalization of the spin-up and spin-down densities. For small concentrations of the spin-down particles (N↓ N↑ ) only the normal state is present and one can ignore the change in the chemical potential μ0↑ of the majority component due to the interaction with the spin-down atoms. In this case, n↑ reduces to the Thomas–Fermi proﬁle (17.7) of an ideal Fermi gas. The density proﬁle of the minority component is instead aﬀected by the interaction with the spin-up atoms. Using the expansion (20.8) one can easily calculate the ﬁrst correction to the equation of state of the spin-down particles. One ﬁnds (μ↓ (r)) = −(3/5)Aμ↑ (r) = −(3/5)A(μ0↑ − Vho (r)), so that the spin-down particles feel ef f an eﬀective potential given by Vho =(1 + 3A/5)Vho , corresponding to renormalized eﬀective oscillator frequencies ωi = ωi0 1 + 3A/5. The conﬁning potential felt by the spin-down atoms is stronger due to the attraction produced by the spin-up atoms. When in the centre of the trap the local concentration of spin-down particles reaches the critical value xc = 0.44 (see previous section) a superﬂuid core starts to nucleate in equilibrium with a polarized normal gas outside the superﬂuid. The radius RSF of the superﬂuid is determined by the equilibrium conditions between the two phases discussed in the previous section (we assume here isotropic trapping in order to simplify the discussion). Towards the periphery of the polarized normal phase the density of the spin-down particles will eventually approach a vanishing value corresponding to R↓ . For even larger values of the radial coordinate, only the density of the spin-up particles will be diﬀerent from zero up to the radius R↑ . In this peripherical region the normal phase corresponds to a fully polarized, noninteracting Fermi gas. By using the Monte Carlo equation of state discussed in the previous section one ﬁnds that the superﬂuid core disappears for polarizations P > Pctrap = 0.77 (Lobo et al., 2006). The sizable diﬀerence between the critical value Pctrap and the value Pc = 0.39 obtained for uniform gases (see previous section) reﬂects the inhomogeneity of the trapping potential. In Figure 20.2 we show the calculated radii of the superﬂuid and of the spin-down and spin-up components as a function of P . The radii are given in units of the noninteracting radius of the majority component R↑0 = aho (48N↑ )1/6 . The ﬁgure explicitly points out the relevant features of the problem. When P → 0 one approaches the standard unpolarized superﬂuid phase, where the three radii (RSF , R↑ 1/4 and R↓ ) coincide with the value ξB R↑0 0.81R↑0 (see eqn (17.12)). By increasing P one

Phase separation in harmonic traps at unitarity

391

1 R 0.8

0.6

R

0.4 RSF 0.2

0

0

0.2

0.4

0.6

0.8

1

P

Figure 20.2 Radii of the three phases in the trap in units of the radius R↑0 = aho (48N↑ )1/6 of a noninteracting fully polarized gas. From Giorgini et al. (2008).

observes the typical shell structure with RSF < R↓ < R↑ . The spin-up radius increases and eventually approaches the noninteracting value when P → 1. The spin-down radius instead decreases and eventually vanishes as P → 1. Finally, the radius RSF of the superﬂuid component decreases and vanishes for Pctrap = 0.77, corresponding to the disappearance of the superﬂuid phase. The predicted value for the critical polarization is in good agreement with the ﬁndings of the MIT experiments (Zwierlein et al., 2006a; Shin et al., 2006), where the interplay between the superﬂuid and the normal phase was investigated by varying the polarization P of the gas (the value of Pctrap is independent of the deformation of the trap, provided one can apply the local density approximation). The experimental evidence for superﬂuidity in a spin-imbalanced gas emerges from measurements of the condensate fraction and of the vortex structure in fast-rotating conﬁgurations (Zwierlein et al., 2006a). Shin et al. (2006) directly measured the in situ density difference n↑ (r) − n↓ (r) with phase contrast techniques. Phase separation was observed by correlating the presence of a core region with n↑ − n↓ = 0 with the presence of a condensate of pairs. At unitarity these results reveal that the superﬂuid core appears for P ≤ 0.75. An interesting quantity that can be directly extracted from these measurements is the doubly integrated density diﬀerence (1) nd (z) = dxdy[n↑ (r) − n↓ (r)], (20.12) which is reported in Figure 20.3 for a unitary gas with P = 0.58. The ﬁgure reveals the (1) occurrence of a characteristic central region where nd (z) is constant. The physical

392

Spin-polarized Fermi Gases 108 atoms/cm 7 6 5 4 3 2 1 –100

–50

50

100

μm

Figure 20.3 Double integrated density diﬀerence measured at unitarity in an ultracold trapped Fermi gas of 6 Li with polarization P = 0.58 (from Shin et al., 2006). The theoretical curves correspond to the theory of Sections 20.3 and 20.4 based on the local density approximation (solid line) and to the predictions of a noninteracting gas with the same value of P (dashed line). From Recati et al. (2008).

origin of this plateau can be understood using the local density approximation (De Silva and Mueller, 2006a; Haque and Stoof, 2006): it is a consequence of the existence of a core region with n↑ (r) = n↓ (r), which is naturally interpreted as the superﬂuid core. Furthermore, the value of z where the density exhibits the small cusp corresponds to the Thomas–Fermi radius RSF of the superﬂuid. In the same ﬁgure we show the theoretical predictions, based on the Monte Carlo results for the equation of state of the superﬂuid and normal phases (solid line), which agree well with the experimental data (Recati et al., 2008). The theoretical predictions discussed above are based on a zero-temperature assumption and on the local density approximation applied to the various phases of the trapped Fermi gas. While the applicability of the LDA seems to be adequate to describe the MIT data, the Rice experiments (Partridge et al., 2006), carried out with a very elongated trap, have revealed the occurrence of important surface tension eﬀects (De Silva and Mueller, 2006b; Haque and Stoof, 2007). Valuable information on the nature of the spin-polarized phase is also provided by its dynamic behaviour. A ﬁrst important case is that of high polarization, where the gas is in the normal phase and, according to the discussion after eqn (20.11), the eﬀective trapping frequency, felt by the minority component, is renormalized by the factor 1 + 3A/5. This results in the value ωidipole

= ωi

3 1+ A 5

m 1.23ωi , m∗

(20.13)

Phase separation in harmonic traps at unitarity

393

with i = x, y, z, for the frequency of the dipole oscillation of the spin-down particles, where we have included an additional eﬀective mass term caused by the interaction with the spin-up particles. In this regime the impurities behave like polarons (see next section). The eﬀective mass m∗ also enters the expansion (20.8). Also, the excitations of higher multipolarity, like the# axial breathing mode of the spin-down particles, will

be aﬀected by the same factor (1 + 35 A) mm∗ with respect to the noninteracting prediction. In the experiment of Nascimbene et al. (2009) the value m∗ /m = 1.17 was extracted from the study of the axial breathing mode of the minority component at unitarity. The same experiment also conﬁrmed that in the regime of high polarization the spin-up component behaves like a noninteracting Fermi gas whose axial breathing frequency is given by the ideal gas value 2ωi . As the polarization of the gas decreases and the system enters the superﬂuid regime below P ∼ 0.77, the dynamic behaviour of the superﬂuid component is governed by hydrodynamic theory. In this case, the axial breathing mode of the minority component is expected to exhibit the same superﬂuid collective frequency as in the absence of polarization. Nascimbene et al. (2009) actually used the sum rule estimate (Menotti and Stringari, 2002) ω 2 = −2

z 2 ∂z 2 /∂ωz2

(20.14)

for the frequency of the axial breathing mode. At unitarity the LDA imposes that the radii scale with the trapping frequencies in the same way as in the ideal Fermi gas, irrespective of the value of polarization. One then ﬁnds the same value ω = 12/5ωz for the frequency of the axial breathing mode, already derived for an unpolarized 2.0

ωCL

ω1 / ωz

1.9 1.8 1.7 1.6 1.5 0.0

ωHD 0.2

0.4

0.6

0.8

1.0

P

Figure 20.4 Frequency of the breathing mode normalized to the axial trapping frequency ωz as a function of the population imbalance. The frequencies in the superﬂuid (ωHD = 12/5 ωz ) and collisionless (ωCL = 2 ωz ) limits are indicated by the dashed lines. The axial (radial) trap frequency is 28.9(1) Hz (420 Hz). From Nascimbene et al. (2009). Reprinted with c 2009, American Physical Society. permission from Physical Review Letters, 103, 170402;

394

Spin-polarized Fermi Gases

Fermi gas in the limit of highly elongated traps (see Section 19.1). Experimentally, the hydrodynamic formula is found to be very accurate except for high values of the polarization, close to the critical value for the transition to the normal phase, where a large damping is observed and the frequency moves towards the collisionless value 2ωz (see Figure 20.4).

20.5

The Fermi polaron

Result (20.8) shows that in the limit of very high polarization the energy of a single spin-down impurity embedded in the Fermi sea of spin-up particles is equal to μ↓ = −(3/5)AEF↑ ∼ −0.6EF↑ at unitarity. The impurity is also characterized by an eﬀective mass m∗ ∼ 1.2m. The negative sign in the energy reﬂects the attractive nature of the force between the impurity and the Fermi sea. The dressed particle is called the Fermi polaron, in analogy with solid-state physics concepts used to describe electrons dressed by optical phonons. The polaron concept is not, of course, limited to the strongly interacting conditions of unitarity. In particular, for a weakly interacting regime of small scattering lengths, one can use perturbation theory, yielding, up to second order in kF a, the results 4kF a 2(kF a)2 + (20.15) μ↓ = −EF↑ 3π π2 and 4 2 m = m 1 + 2 (kF a) . 3π ∗

(20.16)

A nontrivial many-body problem concerns the evaluation of the chemical potential, and the eﬀective mass of the polaron along the whole BEC-BCS crossover as a function of the dimensionless parameter 1/kF a. A very insightful ansatz for the wave function Ψ of the polaron was provided by Chevy (2006b), who suggested the form |k|>kF

|Ψ = φ0 |0↓ |0↑ +

φqk |q − k↓ c†k↑ cq↑ |0↑

(20.17)

|q|k F Γ(ω) = 2πΩ2R ⎣|φ0 |2 δ(ω + μ↓ ) + |φqk |2 δ(ω + μ↓ − k + q − |q−k| )⎦. q Eunif ) is given by g12 < g1 g2 (Colson and Fetter, 1978). On the other hand, the uniform phase described by eqn (21.4) is dynamically stable against local density ﬂuctuations, i.e. (∂ 2 E/∂N12 )(∂ 2 E/∂N22 ) > (∂ 2 E/(∂N1 ∂N2 ))2 , under the more severe condition √ |g12 | < g11 g22 (21.7) involving the modulus of g12 . For trapped conﬁgurations, a useful description of the equilibrium proﬁles n1 (r) = |Ψ1 |2 and n2 (r) = |Ψ2 |2 , with Ψ1 (r, t) = e−iμ1 t/ Ψ1 (r) and Ψ2 (r, t) = e−iμ2 t/ Ψ2 (r), respectively, is provided by the Thomas–Fermi approximation, which consists of neglecting the quantum pressure terms in the Gross-Pitaevskii equations (21.2)–(21.3). Under the miscibility condition (21.7) one ﬁnds μ1 − V1,ext (r) − g11 n1 (r) − g12 n2 (r) = 0

(21.8)

μ2 − V2,ext (r) − g22 n2 (r) − g12 n1 (r) = 0,

(21.9)

and

where, in analogy with the Thomas–Fermi approximation applied to a singlecomponent Gross-Pitaevskii equation (see Section 11.2), the equations hold provided n1 (r) and n2 (r) are positive, otherwise their value should be set equal to zero. In the region where both the solutions n1 and n2 diﬀer from zero the densities take the form 1 g12 μ1 − μ2 − V1,eff (r) (21.10) n1 (r) = g11 (1 − Δ) g22 and 1 n2 (r) = g22 (1 − Δ)

g12 μ2 − μ1 − V2,eff (r) , g11

(21.11)

2 where Δ = g12 /(g11 g22 ) < 1 and the eﬀective external potentials felt by the two components are

V1,eff (r) = V1,ext (r) −

g12 V2,ext (r), g22

(21.12)

V2,eff (r) = V2,ext (r) −

g12 V1,ext (r). g11

(21.13)

and

404

Quantum Mixtures and Spinor Gases

The above equations show that the Thomas–Fermi radii RT F 1 and RT F 2 of the two components are, in general, diﬀerent. Let us suppose, for example, that RT F 1 < RT F 2 . For intermediate values of the spatial coordinate the density of the ﬁrst component is vanishing, while the one of the second component is given by the usual Thomas–Fermi solution n2 (r) = (μ2 − V2,ext (r))/g22 (see eqn (21.9)). An interesting feature exhibited by eqns (21.10)–(21.11) is that, by properly choosing the trapping potential and the value of the coupling constants, it is possible to realize situations where the eﬀective potential acting on one of the two components vanishes due to an exact compensation between the external potential and the interaction with the other component. For example, if V1,ext = V2,ext and g12 = g11 then V2,eff = 0 (see eqn (21.13)). This peculiar situation, which also allows for the realization of uniform conﬁgurations in the presence of external trapping, is not unique of Bose–Bose mixtures, but can also be realized with Bose–Fermi mixtures (see Section 21.5), by suitably tuning the values of the interspecies scattering lengths. One should, however, notice that, when the values of the three coupling constants g11 , g12 , and g22 are very similar, the Thomas–Fermi (TF) results (21.10) and (21.11) are no longer applicable. Let us assume, for example, V1,ext = V2,ext ≡ Vext and g11 ∼ g12 ∼ g22 ∼ g. While the total density n = n1 + n2 is still given by the Thomas–Fermi expression n ∼ (1/g)(μ − Vext ), the determination of the density proﬁles n1 and n2 cannot be inferred from the TF equations, but requires the explicit solution of the coupled Gross-Pitaevskii equations, accounting for quantum pressure eﬀects. This is the case, for example, of the |F = 1, mF = −1 and |F = 2, mF = 1 states (hereafter called |1 and |2) of 87 Rb employed in the experiment by Hall et al. (1998a), where the three coupling constant parameters are very similar. Furthermore, one should recall that in this case the trapping potentials have the same shape because the corresponding Lande factors are equal in modulus but have opposite sign (see Section 9.3). In Figure 21.1 we show the measured density proﬁle of the two hyperﬁne states |1 and |2, corresponding to N1 ∼ N2 . The ﬁgure clearly shows that the two components are separated in space. The crater corresponds to the region occupied by the |2 atoms. This behaviour is consistent with the fact that the scattering length a11 is larger than a22 , and that consequently the atoms |1 like to stay at the periphery. The collective oscillations of interacting mixtures of Bose–Einstein condensates also exhibit interesting features. The frequency of the Bogoliubov modes in uniform conﬁgurations can be calculated by solving the coupled Gross-Pitaevskii equations (21.2)–(21.3) using the ansatz Ψi (r, t) = e−iμi t/ Ψi,0 (r) + ui ei(k·r−ωt) + vi∗ e−i(k·r−ωt) ,

(21.14)

with i = 1, 2. By linearizing the equations of motion around equilibrium, in the case of equal masses m1 = m2 ≡ m we obtain the result (Pethick and Smith, 2008) ωd(s) =

2 k 2 2m

2 k 2 2 + 2mcd(s) , 2m

(21.15)

Mixtures of Bose–Einstein condensates

405

(a)

(b) (c)

Figure 21.1 Measured density proﬁle of a 87 Rb mixture of the two hyperﬁne states (a) |1 and (b) |2 . The crater corresponds to a region occupied by the |2 atoms. In (c), by introducing a nonzero relative gravitational sag, one observes a shift of the centre of the crater. From Hall et al. (1998a). Reprinted with permission from Physical Review Letters, 81, c 1998, American Physical Society. 1539;

with the density (d) and spin (s) sound velocities given by

c2d(s)

=

g11 n1 + g22 n2 ±

2 (g11 n1 − g22 n2 )2 + 4n1 n2 g12 . 2m

(21.16)

The sign +(−) in the above equations corresponds to ‘density’ (‘spin’) oscillations, where the two ﬂuids move in phase (out of phase). In the case of equal coupling constants (g11 = g22 = g12 ) and equal densities (n1 = n2 ) the spin velocity vanishes and the dispersion takes the quadratic form ω = k 2 /2m (Colson and Fetter, 1978). An interesting question concerns the stability of the system in the presence of uniform currents. While for a single Bose gas the condition of stability reduces to the famous Landau criterion (6.4), yielding the velocity of sound for the critical velocity, in the presence of two ﬂuids the situation is richer. By considering a mixture where the ﬂuids move with diﬀerent velocities v1 and v2 , one in fact ﬁnds that novel conditions are required in order to ensure stability. The problem is easily solved for two uniform ﬂuids with the same densities (n1 = n2 = n/2), the same masses, and symmetric values for the coupling constants (g11 = g22 ≡ g). In this case the sound

406

Quantum Mixtures and Spinor Gases

velocity, providing the leading term in the Bogoliubov dispersion relations at small wave vectors k, takes the simple expression (see, for example, Suzuki et al., 2010) # 1 2 c = c20 + v 2 ± c20 v 2 + c40 g12 /g 2 ± V, (21.17) 4 where c20 = gn/2m, v = v1 − v2 is the relative velocity between the two ﬂuids and V is the modulus of the centre-of-mass velocity V = (v1 + v2 )/2. In deriving eqn (21.17) we have also assumed that the vectors v1 , v2 , and k are directed along the same axis. The term ±V provides the Doppler eﬀect responsible for the instability associated with the Landau criterion if c becomes negative (energetic instability). The relative velocity v has instead a deeper consequence on the propagation of sound. In fact, one can easily see that in the interval c < |v|/2 < c , where c = (g − g12 )n/2m and s d s cd = (g + g12 )n/2m in the considered symmetric case, the solution (21.17) takes an imaginary value corresponding to the emergence of dynamic instability. For values of v larger than cd the sound velocity is real. However, in this case the system develops a dynamical instability for larger values of k, beyond the phonon regime. In the case of symmetric mixtures of 87 Rb, with atomic gases occupying the hyperﬁne states |F = 1, mF = −1 and |F = 2, mF = 1 and equal population, the dynamic instability takes place for very small values of v as a consequence of the smallness of the spin sound velocity cs . The critical velocity becomes larger in the case of imbalanced populations. The occurrence of such an instability was shown experimentally by Hamner et al. (2011), who pointed out the emergence of a rapid growth of large-amplitude modulations in the form of trains of dark–bright solitons. Collective oscillations involving mixtures of Bose–Einstein condensed gases can also be studied in the presence of harmonic trapping by generalizing the hydrodynamic formalism developed in Section 12.2 to the case of a spin mixture. In the simplest case of symmetric conﬁgurations (N1 = N2 and g11 = g22 ≡ g > |g12 |) the equation for the density oscillations keeps the same form (12.9) as for a single Bose–Einstein condensate with c2 = (g + g12 )n/2. The equation for the spin density ﬂuctuations δs(r) = δn↑ (r) − δn↓ (r) is instead modiﬁed and takes the form m

g − g12 ∂2 ∇ · [n(r)∇δs(r)]. δs(r) = 2 ∂t 2

(21.18)

Since the equilibrium density proﬁle has the form n(r) = 2(μ − V ext (r))/(g + g12 ), all the discretized frequencies are simply renormalized by the factor (g − g12 )/(g + g12 ) with respect to the values predicted for a single Bose–Einstein condensate (see Section 12.2). For example, the frequency of the most relevant spin dipole (SD) oscillation, where the two spin clouds move rigidly with opposite phase, takes the expression g − g12 ωSD = ωho . (21.19) g + g12 The SD oscillation is the analogue of the famous giant dipole resonance of nuclear physics, where neutrons and protons oscillate with opposite phase (Bohr and Mottelson, 1969).

Spinor Bose–Einstein condensates

407

For g12 = g, N1 = N2 and equal external potentials, the hydrodynamic picture breaks down and one should solve the full Gross-Pitaevskii equations. The problem was discussed by Sinatra et al. (1999) who derived the following equation for the spin oscillations: 2 2 − ∇ + Vext (r) + gn(r) − μ δΨ = ωδΨ, (21.20) 2m where δΦ is the relative change of the order parameter occurring during the oscillation. In the Thomas–Fermi limit the eﬀective potential entering the above equation is very ﬂat in the interior region and grows rapidly like Vext − μ outside. The lowest-energy solutions are consequently well approximated by free particles with wave vectors of 2 the order of q ∼ 1/R, corresponding to excitation frequencies ωho /μ ωho . Due to the softness of these oscillations, even small eﬀects, like the displacement between the centres of the two potentials, or small diﬀerences between the coupling constants, can have dramatic consequences on the relative motion of these binary mixtures. Furthermore, these oscillations are highly sensitive to nonlinear eﬀects.

21.2

Spinor Bose–Einstein condensates

In this section we consider atoms occupying single-particle states with angular momentum F = 0. In the absence of external magnetic ﬁelds the Hamiltonian of the system is invariant with respect to rotations in spin space. Experimentally, these conﬁgurations can be realized with optical traps. In Section 21.1 we considered a mixture of 87 Rb atoms occupying hyperﬁne states with diﬀerent values of F . In this case rotational invariance is destroyed. The total spin of the atom is the sum of a nuclear (I) and of an electronic spin which, for alkali atoms, is S = 1/2. The orbital angular moment is zero and F is often called the hyperﬁne spin. For bosons the possible values of F include all the integers from |I − S| to I + S. For simplicity we will consider here only the case F = 1. In the case of weakly interacting bosons only collisions with relative orbital angular momentum l = 0 are important. As a consequence, only scattering states with total angular momentum of even parity are allowed. This means that for two identical atoms with F = 1, the possible values of total angular moment taking part in the s-wave scattering are 0 and 2. The corresponding collisional scattering lengths are labelled with a0 and a2 , respectively, and their values are known for several atomic species with F = 1: 7 Li, a0 = 23.9, a2 = 6.8; 23 Na, a0 = 50.0, a2 = 55.0; 41 K, a0 = 68.5, a2 = 63.5; and 87 Rb, a0 = 101.8, a2 = 100.4, with the values given in units of the Bohr radius aB . In the following we brieﬂy discuss the behaviour of the many-body ground state of F = 1 spinor condensates in the case of uniform conﬁgurations. We will employ a mean-ﬁeld picture (Ho, 1998; Law et al., 1998; Ohmi and √ Machida, 1998) where the condensate wave function is written in the form |Ψ (σ) = n|χ(σ), with the spinor component χ given by |χ (σ) = (χ1 , χ0 , χ−1 ), normalized to unity: χ(σ)|χ(σ) = σ χ∗σ χσ = 1.

(21.21)

408

Quantum Mixtures and Spinor Gases

The mean-ﬁeld energy describing our spinor condensates generalizes the Bogoliubov expression (4.10) (E = N ng/2 = 2π2 an2 /m ) to include the presence of the two scattering lengths introduced above. By properly taking into account the spin structure characterizing the eﬀective two-body interaction potential to be used in the mean-ﬁeld picture, the energy takes the useful form E=

1 2 N n c0 + c2 |χ |F| χ| , 2

(21.22)

where c0 = (g0 + 2g2 ) /3 and c2 = (g2 − g0 ) /3 with gi = 4π2 ai /m, and F is the hyperﬁne spin operator. If c2 is negative (this is the case of 7 Li, 41 K, and 87 Rb) the energy functional favours ferromagnetism. Correspondingly, the ground state is |χ(σ) = (1, 0, 0) or (0, 0, 1) and 2 |χ |F| χ| = 1. If instead c2 > 0, which is the case of 23 Na, the ground state has an antiferromagnetic nature. can take the longitudinal (0, 1, 0) The corresponding spinor 2 or transverse 1, 0, eiφ polar form, and |χ |F| χ| = 0. In both cases we have chosen the quantization axis along z. Of course, in the absence of an external magnetic ﬁeld the direction of the z-axis is arbitrary and the spinor is deﬁned up to an arbitrary rotation in spin space. In order to describe the behaviour of the spinor BEC in an external magnetic ﬁeld we should add ﬁeld-depending terms into the energy. These terms violate the rotational invariance of the Hamiltonian. Taking into account the ﬁrst two terms in the expansion with respect to a uniform magnetic ﬁeld B, directed along the z-direction, we can write the energy of the system as E=

1 2 2 N n c0 + c2 F + p Fz + q Fz , 2

(21.23)

which generalizes eqn (21.22). The factors p and q are diﬀerent for diﬀerent atoms and, to some extent, can be tuned at will. The inclusion of the new terms makes the phase diagram very rich and was investigated experimentally by Stenger et al. (1998). Various phase transitions have been predicted and observed as a function of q both for ferromagnetic ( c2 < 0) and antiferromanagnetic (c2 > 0) coupling. Actually, for ﬁnite p and q > 0 the ground state can correspond to the longitudinal ferromagnetic states (1, 0, 0) or (0, 0, 1), or to the longitudinal polar state (0, 1, 0), depending on the value of p and q. It is also interesting to discuss the ferromagnetic and antiferromagnetic behaviour of these S = 1 states in terms of their miscibility and immiscibility. For a homogeneous two-component (a and b) system, the mean-ﬁeld energy can be written in the form (1/2) dr(gaa n2a + gbb n2b + 2gab na nb ) and, as discussed in Section 21.1, the criterion for √ √ miscibility (immiscibility) is gab < gaa gbb (gab > gaa gbb ). In the case of the S = 1 spinors the coupling constants gij characterizing the interaction between the various spin components can easily be calculated starting from eqn (21.22), making explicit use of the 3 × 3 matrix structure of the spin operator F. For a mixture of the mF = ±1 states one ﬁnds g+1,+1 = g−1.−1 = c0 + c2 and g+1,−1 = c0 . For a mixtures of the

Coherently coupled Bose–Einstein condensates

409

mF = + 1 and mF = 0 states one instead ﬁnds g+1,+1 = g+1,0 = c0 + c2 and g0,0 = c0 . For an antiferromagnetic interaction (c2 > 0) one then ﬁnds that the states mF = ±1 are miscible while the states mF = +1 (or mF = −1) and mF = 0 are immiscible. The opposite happens for a ferromagnetic interaction. The miscibility properties of the various spinor states were ﬁrst investigated experimentally in the works by Stenger et al. (1998) and Miesner et al. (1999), conﬁrming the antiferromagnetic nature of the S = 1 spinor condensates in 23 Na. For a recent exhaustive review of spinor condensates, including discussion of their dynamic and thermodynamic properties, see Stamper-Kurn and Ueda (2013).

21.3

Coherently coupled Bose–Einstein condensates

Equations (21.2)–(21.3) conserve the numbers of atoms of each component. However, the application of an oscillating radiofrequency (rf) ﬁeld tuned close to the hyperﬁne splitting Vhf can result in the possibility of transfer of atoms from one state to the other. This process can be described by adding a term proportional to Ψ2 to the equation for Ψ1 , and vice versa. In the rotating wave approximation we ﬁnd 2 2 ∂ ∇ Ω(t) iωrf t 2 2 + Vext (r) + g11 |Ψ1 | + g12 |Ψ2 | Ψ1 − e i Ψ1 = − Ψ2 (21.24) ∂t 2m 2 and ∂ i Ψ2 = ∂t

2 2 ∇ Ω (t) −iωrf t 2 2 + Vext (r) + Vhf + g22 |Ψ2 | + g12 |Ψ1 | Ψ2 − e − Ψ1 , 2m 2 (21.25)

where ωrf is the frequency of the rf wave and the Rabi energy Ω(t) plays the role of the coupling constant for the transition. Notice that the phase of Ω deﬁning the phase of the rf ﬁeld is arbitrary. In the following, Ω will be assumed real and positive. For simplicity, we have assumed that the external potential felt by the two spin components is the same, apart from the hyperﬁne splitting Vhf ﬁxed by the magnetic ﬁeld. Notice that the physical meaning of the amplitude Ω is diﬀerent for diﬀerent types of transitions. If the transfer can be obtained via one-photon transitions, Ω is proportional to the ﬁeld amplitude. However, in other cases the transition requires two units of angular momentum and can only be activated with two-photon transitions. In this case the amplitude Ω is quadratic in the rf ﬁeld. Starting from a conﬁguration where initially all the atoms are in |1 (and hence √ Ψ0 = n0 ), an rf pulse of short duration will bring some atoms into state |2 without changing their space distribution. In this case, one can write the solutions of the Gross-Pitaevskii equations in the form Ψ1 (r, t) = A1 (t) n0 (r) , Ψ2 (r, t) = A2 (t) n0 (r). (21.26) By further assuming g11 ∼ g22 ∼ g12 , the equations for the amplitudes A become Ω iA˙ 1 = μ1 A1 − eiωrf t A2 , 2

Ω iA˙ 2 = μ2 A2 − e−iωrf t A1 , 2

(21.27)

410

Quantum Mixtures and Spinor Gases

where μ1 and μ2 = μ1 + Vhf are the chemical potentials of the two components. For brief pulses of duration t such that t 1/δ, where δ = ωrf − Vhf / Vhf /, the solution takes the form A1 = e−iμ1 t/ C1 e−iΩt/2 + C2 e+iΩt/2 , A2 = e−iμ2 t/ −C1 e−iΩt/2 + C2 eiΩt/2 , (21.28) where C1 and C2 are ﬁxed by the initial conditions (C1 = C2 = 1/2 in our case). 2 2 Then, after the time τ = π/2Ω (‘π/2 pulse’), one gets |A1 | = |A2 | = 1/2 and the atoms will be equally distributed between the two hyperﬁne states. A pulse of double duration (‘π pulse’) will instead completely convert the system from state |1 into |2. However, if the π pulse is split into two π/2 pulses with an intermediate time delay t0 , the wave functions of the condensates, after the ﬁrst pulse, will evolve according to the laws A1 ∼ e−iμ1 t/ and A2 ∼ e−iμ2 t/ . As a consequence, after the time t0 the relative phase between the two condensates has varied by the amount (μ1 − μ2 )t0 /. On the other hand, in the same time interval the phase of the coupling ﬁeld has also evolved by the amount ωrf t0 . One can see that the fraction of atoms which after the second π/2 pulse will be converted to state |2, is given by ,

N μ2 − μ1 N2 = 1 + cos ωrf − t0 . (21.29) 2 Since the diﬀerence between the two chemical potentials coincides with the hyperﬁne splitting (μ2 − μ1 = Vhf ), the frequency of the oscillation is given by the detuning δ = ωrf − Vhf /. In Figure 21.2 we show the measured population transfer as a function of the separation time t0 between two π/2 pulses (Hall et al., 1998b). The oscillation in the ﬁnal occupation number in the |2 state is in good agreement with the prediction (21.29). This experiment provides an important check of the general law Ψ0 (t) ∼ e−iμt/ Ψ0 (0) governing the time evolution of the order parameter of Bose–Einstein condensates. If all the atoms are converted into the second state with a π pulse, other interesting phenomena may occur on a longer time scale which are the consequence of interaction eﬀects. Let us suppose that initially the system is in equilibrium in state |1. After the π pulse the system will no longer be in equilibrium, unless the scattering length a22 is exactly equal to a11 , and consequently will start oscillating with the typical frequencies of the collective modes. Since the trapping potential is not isotropic the resulting oscillation will be a superposition of the two m = 0 modes (12.15). This is actually what is observed experimentally (see Figure 21.3, where the measured axial and radial sizes are shown as a function of the time interval after the application of the π pulse). The data show that the amplitude of the oscillation is rather small, revealing that, as expected, a22 is not very diﬀerent from a11 . The oscillations can be calculated theoretically by solving the time-dependent equations of motion and by treating the value of the scattering length a22 as a ﬁtting parameter. The experimental points are well reproduced by the value a11 /a22 = 1.062(12). This result provides a precise determination of the small diﬀerences between the two scattering lengths.

Coherently coupled Bose–Einstein condensates

411

100%

Fraction in|2

75%

50%

25%

0%

0

2

4 6 8 Pulse separation [ms]

10

12

Figure 21.2 Population transfer from |1 to |2 resulting from twin π/2 pulse coupling, as a function of the delay between the two pulses. The ﬁrst pulse prepares the condensate in an equal superposition of the two states. The second pulse induces further population transfer, which is sensitive to the relative phase that has evolved during the pulse separation time. From Cornell et al. (1998). Reprinted with permission from Journal of Low Temperature c 1998, Springer. Physics, 113, 151; 56 Axial

Radial

72

Size [μm]

54 70 52 68 50 66

0

1

2 3 Time [units of ωr–1]

4

0

1

2 3 Time [units of ωr–1]

4

Figure 21.3 Oscillation in the width of the cloud in both the (a) axial and (b) radial directions due to the instantaneous change in scattering length in the experiment of Matthews et al. (1998). Time is measured in units of ωr ≡ ω⊥ = 9.4 ms. The solid lines are the time-dependent widths calculated using eqns (12.42) and (12.43) (see text).

412

Quantum Mixtures and Spinor Gases

It is also interesting to discuss the solutions of the Gross-Pitaevskii equations (21.24)–(21.25) in the presence of stationary rf coupling between the two hyperﬁne states. To this purpose it is convenient to introduce a unitary transformation yielding Ψ1 → e−iωrf t/2 Ψ1 and Ψ2 → e+iωrf t/2 Ψ2 , corresponding to a rotation in spin space around the third spin axis by the angle ωrf t. The new Hamiltonian in the rotated frame becomes time independent and, setting the rf frequency equal to the hyperﬁne splitting (ωrf = Vhf ), the Gross-Pitaevskii equations take the form 2 2 ∂ ∇ Ω 2 2 + Vext (r) + g11 |Ψ1 | + g12 |Ψ2 | Ψ1 − Ψ2 i Ψ1 = − (21.30) ∂t 2m 2 and i

∂ Ψ2 = ∂t

2 2 ∇ Ω 2 2 + Vext (r) + g22 |Ψ2 | + g12 |Ψ1 | Ψ2 − Ψ1 . − 2m 2

(21.31)

These equations can also be derived starting from the energy functional (21.1) containing the additional rf term Ω Erf = − dr (Ψ∗1 Ψ2 + Ψ∗2 Ψ1 ) = −Ω dr|Ψ1 ||Ψ2 | cos(φ2 − φ1 ) , (21.32) 2 which depends explicitly on the relative phase (φ2 − φ1 ) between the two order parameters. The blocking of the relative phases implies that the relative number N1 − N2 of atoms in the two spin states is not conserved and obeys the following equation: d(N1 − N2 ) = Ω |Ψ1 ||Ψ2 | sin(φ2 − φ1 ) dr. dt The ground state of the mixture corresponds to the condition φ1 = φ2 for the two phases and, if g11 = g22 ≡ g, to N1 = N2 and equal values n1 (r) = n2 (r) for the densities. The fact that the energy depends explicitly on the relative phase has a crucial consequence on the dynamic properties of the system. The existence of gapless excitations in uniform matter is ensured by a spontaneous breaking of gauge symmetry. This is the case for the in-phase mode where the two phases of the order parameter are equal, but is violated for the spin modes where the relative phase is locked energetically by the Rabi term. Actually, the explicit solution of the linearized time-dependent Gross-Pitaevskii equations in uniform matter yields the following expressions for the dispersion of the two Bogoliubov modes (see, for example, Abad and Recati, 2013):

k 2 (g + g12 )n k 2 ωd = + (21.33) 2m 2m and

ωs =

k 2 +Ω 2m

k 2 (g − g12 )n +Ω+ . 2m

(21.34)

Coherently coupled Bose–Einstein condensates

413

The sound velocity of density waves, derivable from eqn (21.33), coincides with result (21.16), calculated in the absence of Rabi coupling after setting n1 = n2 and g11 = g22 , while in the spin channel the dispersion is aﬀected by the Rabi coupling and turns out to be gapped at k = 0. Equation (21.34) also shows that the Rabi coupling favours the stability of the mixture, which can be even ensured for values of g12 > g, provided the condition Ω > (g12 − g)n is satisﬁed. To better understand the physical meaning of the mode (21.34) let us consider a uniform oscillation with k = 0. Then,

ωs =

(g − g12 )n +Ω Ω.

(21.35)

This equation diﬀers only in notation from the Josephson equation (15.50). This permits us to identify Ω as δJ / and (g −g12 )n as N EC /2. Accordingly, the dimensionless parameter Λ introduced in eqn 15.52 can be identiﬁed as Λ = (g − g12 )n/Ω. Actually, eqn (21.35) describes the internal Josephson eﬀect, already mentioned at the end of Section 15.3. Of course, one can reduce the energy of the mixture to the form (15.48) by direct calculation. The dependence of the energy (21.32) on the relative phase φ2 − φ1 is at the origin of other interesting features, associated with the occurrence of vortical conﬁgurations. Due to the rf coupling, vortices in these spinor conﬁgurations can actually exist in pairs (one for each spin component) and the plane separating the two vortex lines gives rise to a domain wall across which the relative phase of the two condensates changes by 2π. The properties of these vortical solutions, also called vortex molecules, were discussed by Son and Stephanov (2002), who predicted the phenomenon of vortex conﬁnement, in analogy with the quark conﬁnement in the theory of strong interactions (quantum chromodynamics). A simple description of the domain wall can be obtained by looking at the solutions of the coupled Gross-Pitaevskii equations (21.30)–(21.31) in the limit of large length scales, where the densities n1 and n2 can be regarded as uniform and the only important degrees of freedom are the phases φ1 and φ2 . In this limit the energy of the system, apart from a constant term, is a functional of the two phases given by (we assume here n1 = n2 ≡ n/2) n E[φ1 , φ2 ] = 2

2

dr

2 2m

dφ1 dz

2

+

dφ2 dz

2

3 − Ω cos (φ1 − φ2 ) ,

(21.36)

yielding the following diﬀerential sine-Gordon like equation 2 d2 φ1 2 d2 φ2 = − = −Ω sin(φ2 − φ1 ). m dz 2 m dz 2

(21.37)

One should solve this equation with the boundary condition that both φ1 and φ2 approach a constant value as z → ±∞. The trivial solution φ2 = φ1 = const corresponds to the lowest-energy solution of the Gross-Pitaevskii equations which is free of defects.

414

Quantum Mixtures and Spinor Gases

A nontrivial solution, corresponding to an inﬁnite domain wall located at z = 0, is given by

z φ2 = − φ1 = 2 arctan exp , (21.38) ξph where ξph =

2mΩ

(21.39)

is a typical length characterizing the width of the domain wall. When one moves from z = −∞ to +∞ the relative phase φ2 − φ1 changes from −π to π in a space interval of size ξph . The tension of the wall, i.e. the energy per unit area, is obtained by substituting eqn (21.38) into (21.36). One ﬁnds (Son and Stephanov, 2002) σ = 23/2

3/2 n 1/2 Ω . m1/2

(21.40)

The presence of a domain wall attached to a vortex line has important consequences for the circulation properties of the vortex line. Let us suppose that the wave function Ψ1 contains a vortex line with a single unit of quantum circulation, corresponding to a change of its phase by 2π along a closed contour containing the vortex line and crossing the wall. Let us now consider the evolution of the phase of the two condensates along the same contour. Far from the wall one has φ2 = φ1 and both phases acquire a factor π on the path outside the wall. According to eqn (21.38) the phases of the wave functions φ1 and φ2 exhibit a jump equal to π and −π, respectively, across the wall, and consequently the circulation of the wave function Ψ2 around the same closed contour will be exactly zero. In other words, in the presence of the domain wall, the vortex line corresponds to a ﬁnite circulation for only one condensate. For this reason the above conﬁguration is often called half-vortex. In a ﬁnite system, the domain wall can connect two parallel vortex lines, relative to the two condensates, respectively, and is responsible for their relative attraction. Numerical results for the structure of these vortex molecules, based on the full solution of the Gross-Pitaevskii equations, were obtained by Kasamatsu et al. (2004). Experimentally, vortex molecules could be created by a proper rotation of the conﬁning trap, in analogy with the creation of vortices for single Bose–Einstein condensates (see Section 14.6).

21.4

Synthetic gauge ﬁelds and spin-orbit coupling

In charged systems (electrons) the orbital coupling with external magnetic ﬁelds is at the origin of many important phenomena caused by the Lorentz force, where the gauge ﬁelds play a very important role. In atomic gases this possibility is ruled out because of their neutrality. However, an eﬀective gauge ﬁeld can also be produced in neutral systems by rotating the conﬁning trap, and this method has proven very eﬃcient for the creation of quantized vortices (see Chapter 14). The use of optically

Synthetic gauge ﬁelds and spin-orbit coupling

415

dressed states, either employing Raman transitions between diﬀerent hyperﬁne states or shaking a periodic optical lattice (Zenesini et al., 2007; Struck et al., 2011 and 2012; Aidelsburger et al., 2011 and 2013; Miyake et al., 2013), oﬀers alternative possibilities, giving rise to eﬀective gauge ﬁelds as well as to novel spin-orbit-coupled conﬁgurations. In the following we will consider a simple realization of spin-orbit coupling obtained employing Raman transitions. This example is very instructive and has already been implemented experimentally (Lin et al., 2009). In the previous section we discussed some important consequences associated with the coherent coupling between diﬀerent hyperﬁne states induced by rf transitions. The coupling between these states can also be produced via Raman transitions, through the additional transfer of a large amount of momentum from the laser ﬁelds to the atoms involved in the transition. A simple scheme of this Raman process is presented in Figure 21.4, where it is shown that, through a proper choice of the nonlinear Zeeman ﬁeld separating diﬀerent hyperﬁne states and a suitable choice of the frequency diﬀerence ΔωL between the two laser ﬁelds, it is possible to produce eﬃcient transitions involving only two hyperﬁne states. This condition is realized when the detuning is very close to the hyperﬁne splitting between the two states and diﬀers signiﬁcantly from the splittings between other hyperﬁne states, as a consequence of the nonlinearity of the Zeeman eﬀect. It gives rise to a typical spin-1/2 conﬁguration which can be represented by the single-particle spinor Hamiltonian h0 =

Ω p2 Ω ωZ + σx cos(2k0 x − ΔωL t) + σy sin(2k0 x − ΔωL t) − σz , 2m 2 2 2

(21.41)

where ωZ is the Zeeman shift between the two spin states in the absence of Raman coupling, k0 is the modulus of the wave vector diﬀerence (here chosen along

BEC

ħδ/2 ħωz

|−1 = ħδ/2 |0 = ħωq + 3ħδ/2 |+1

Figure 21.4 Level diagram. Two Raman lasers with orthogonal linear polarizations couple the two states |↑ = |mF = 0 and |↓ = |mF = −1 of the F = 1 hyperﬁne manifold of 87 Rb, which diﬀer in energy by a Zeeman splitting ωZ . The lasers have frequency diﬀerence ΔωL = ωZ + δ, where δ is a small detuning from the Raman resonance. The state |mF = 1 can be neglected since it has a much larger detuning, due to the quadratic Zeeman shift ωq .

416

Quantum Mixtures and Spinor Gases

the x-direction) between the two laser ﬁelds characterized by orthogonal linear polarization, while σk , with k = x, y, z, are the usual 2 × 2 Pauli matrices. The Hamiltonian (21.41) is not translationally invariant, but exhibits a peculiar screwlike symmetry, being invariant with respect to helicoidal translations of the form eid(px −k0 σz )/ , consisting of a combination of a rigid translation by the distance d and a spin rotation by the angle −2dk0 around the z-axis. Let us now apply to the wave function the unitary transformation eiΘσz /2 , corresponding to a position and time-dependent rotation in spin space by the angle Θ = 2k0 x − ΔωL t. In the rotating wave approximation, the single-particle Hamiltonian (21.41) is transformed into the translationally invariant and timeindependent form

hSO = 0

Ω 1 δ 2 (px − k0 σz ) + p2⊥ + σx + σ z , 2m 2 2

(21.42)

where the spin-orbit nature acquired by the Hamiltonian results from the non commutativity between the kinetic energy and the position-dependent rotation, while the renormalization of the eﬀective magnetic ﬁeld δ = ΔωL − ωZ results from the additional time dependence exhibited by the wave function in the spin-rotated frame. The same unitary transformation, for k0 = 0, coincides with the transformation bringing the time-dependent eqns (21.24)–(21.25) into the time-independent eqns (21.30)–(21.31). The new Hamiltonian (21.42) is characterized by equal contributions of the Rashba (Bychkov and Rashba, 1984) and Dresselhaus (Dresselhaus, 1955) couplings, currently used in solid-state physics. It is worth noticing that the canonical momentum px = −i∂x entering the new Hamiltonian does not coincide with the physical momentum of particles because of the presence of the spin term k0 σz . For example, the velocity of the spin-up and spin-down particles along x is given by (vx )± = (px ∓ k0 )/m. It is also useful to remark that the unitary transformation eiΘσz /2 , used to derive the spin-orbit Hamiltonian (21.42) starting from eqn (21.41), does not aﬀect the density n(r), nor the z-component s(r) ≡ n↑ (r) − n↓ (r) of the spin density. These densities can consequently be safely calculated using the Hamiltonian (21.42). It is now instructive to discuss the symmetry properties of the spin-orbit Hamiltonian (21.42). (a) Diﬀerently from the Hamiltonian (21.41) deﬁned in the laboratory frame, hSO is translationally invariant. This means that the emergence of density 0 modulations in the ground state (stripes—see discussion below) is the result of a spontaneous breaking of translational symmetry. (b) The spin-orbit Hamiltonian hSO 0 breaks both time reversal and parity symmetry. As we will show later, this is the origin of the breaking of the usual symmetry ω(k) = ω(−k) characterizing the excitation spectrum of most many body systems. (c) The spin-orbit Hamiltonian hSO breaks 0 Galilean invariance. This is best understood by calculating how the spin-orbit Hamiltonian (21.42) is transformed by the unitary Galilean transformation G = eimvx/ which provides a displacement mv of the wave function in momentum space along the x-direction.

Synthetic gauge ﬁelds and spin-orbit coupling

417

Only the x-component of the kinetic energy term is modiﬁed by the transformation, and takes the form 1 −1 1 G (px − k0 σz )2 G = (px − k0 σz + mv)2 , 2m 2m

(21.43)

so that the spin-orbit Hamiltonian (hSO ) = G−1 hSO G, in the new frame, is given by 1 (hSO ) = hSO + mv 2 + mv(px − k0 σz ). 2

(21.44)

The operator (px − k0 σz ), which represents the physical momentum, is not a constant of motion because of the presence of the Raman coupling Ωσx , which does not commute with it. As a consequence, the two Hamiltonians hSO and (hSO ) are physically diﬀerent, yielding a violation of Galilean invariance. The absence of Galilean invariance has deep consequences on the Landau criterion of superﬂuidity (see Section 6.1). It has been shown that in these systems the usual Landau criterion for stability, which applies to the motion of an impurity in the medium, cannot be used to determine the stability of conﬁgurations carrying a supercurrent, the corresponding critical velocities being dramatically diﬀerent (Zhu et al., 2012; Zheng et al., 2013). Ozawa et al. (2013) have furthermore shown that, as a consequence of the lack of Galilean invariance, supercurrents can become dynamically unstable even in a uniform system. In terms of the canonical momentum p, the single-particle eigenvalues of (21.42) are given by 2 δ p2x + p2⊥ Ω2 k0 px ± (p) = + Er ± − , (21.45) + 2m m 2 4 Er = (k0 )2 /2m being the recoil energy, and exhibit a typical double-branch structure, reﬂecting the spinor nature of the conﬁguration. The dispersion of the lower branch, as a function of px , is characterized by the occurrence of a double minimum for small values of Ω and δ. For large values of Ω (much larger than the recoil energy Er ) the lower branch instead exhibits a single-minimum structure of the form =

1 2 1 p + (px + k0 δ/Ω)2 + constant . 2m ⊥ 2m

(21.46)

As shown by the explicit form of the single-particle Hamiltonian (21.42) and by the corresponding dispersion (21.45), the Raman coupling discussed above is well suited to generating eﬀective gauge potentials and spin-orbit-coupled conﬁgurations. This procedure has been implemented experimentally (Lin et al., 2009) to generate an eﬀective Lorentz force, causing the appearance of quantized vortices in Bose–Einstein condensates (see Figure 21.5). The Lorentz force is in practice realized by introducing a space dependence in the Zeeman splitting and hence in the resulting detuning δ. By making the choice δ = αy the dispersion (21.46) exhibits a typical gauge ﬁeld Ax = −(αk0 /Ω)y, responsible for an eﬀective uniform magnetic ﬁeld B = αk0 /Ω

418

Quantum Mixtures and Spinor Gases (a)

δ' = 0

(b)

δ' = 0.13 kHz μm–1

(c)

(d)

δ' = 0.31 kHz μm–1

(e)

δ' = 0.34 kHz μm–1

(f)

δ' = 0.27 kHz μm–1

Y position after TOF [μm]

80

0

–80 δ' = 0.40 kHz μm–1

80

0

–80 –80

0

80

–80 0 80 X position after TOF [μm]

–80

0

80

Figure 21.5 Appearance of vortices in a spin-orbit-coupled BEC at diﬀerent detuning gradients. Data was taken for N = 1.4 × 105 atoms at hold time th = 0.57 s. (a)–(f ): Images of the |mF = 0 component of the dressed state after a 25.1 ms TOF with detuning gradient δ from 0 to 0.43 kHz μm−1 at Raman coupling ΩR = 8.20 EL . From Lin et al. (2009). c Macmillan Publishers Ltd. Reprinted with permission from Nature, 462, 628;

oriented along the z-direction. By engineering more complex laser conﬁgurations it is possible to design even richer situations, giving rise to non-abelian gauge ﬁelds, like the Rashba coupling, responsible for novel topological features (for recent reviews see Dalibard et al. (2011), Galitski and Spielman (2013), and Zhai (2014)). In the following we will investigate some consequences of the spin-orbit Hamiltonian (21.42) on the many-body quantum phases of a Bose–Einstein condensate in the simplest case of vanishing detuning δ. In this case, the single-particle dispersion (21.46), for Ω < 4Er , exhibits two symmetric minima at momenta px = ±k1 with k1 = k0 1 − (Ω/4Er )2 , both capable of hosting a Bose–Einstein condensate. For larger values of Ω (Ω > 4Er ), the dispersion instead exhibits a single minimum at px = 0. The eﬀective mass 1/m∗ = d2 /dp2x of particles moving along the x-direction exhibits a nontrivial Ω dependence. Near the minimum, i.e. setting px = k1 , one ﬁnds (Zheng et al., 2013) m =1− m∗

Ω 4Er

2 for Ω < 4Er

(21.47)

and m 4Er for Ω > 4Er . =1− ∗ m Ω

(21.48)

Synthetic gauge ﬁelds and spin-orbit coupling

419

The eﬀective mass exhibits a divergent behaviour at Ω = 4Er when the double-well structure disappears and the dispersion takes a p4x law near the minimum. As we will show below the double-well structure exhibited by the single-particle dispersion is at the origin of new interesting features exhibited by the solution of the many-body problem. In uniform matter one can use the ansatz (Li et al., 2012)

√ cos θ sin θ ik1 x −ik1 x Ψ (r) = n (21.49) ¯ C+ + C− e e − sin θ − cos θ for the ground sta