Quantum Entanglement and the Geometry of Spacetime

Transcription

1 Quantum Entanglement and the Geometry of Spacetime Matthew Headrick Brandeis University UMass-Boston Physics Colloquium October 26, 2017 It from Qubit Simons Foundation

2 Entropy and area Bekenstein-Hawking 74: kb c3 area(horizon) area(horizon) S= = kb 2 4GN ~ 4lP GN gravity Planck length ( cm) ~ quantum mechanics kb statistical mechanics What are the atoms of the black hole? Why is S area?

3 Entropy and area In any number d of dimensions, G N ~ has units of area ( L d 1 ) Natural unit in quantum gravity is Planck area Generalizations of Bekenstein-Hawking: De Sitter spacetime (Gibbons-Hawking 77): Holographic entropy bounds (Bekenstein 81, Bousso 99): for arbitrary closed surface in arbitrary spacetime How general is the area-entropy relation? What is its origin? clue: Holographic entanglement entropy (Ryu-Takayanagi 06) Vast but also limited generalization of Bekenstein-Hawking S = area(horizon) 4G N ~ To understand it, we first need to extend our notion of entropy S apple area 4G N ~ Jacobson 94 used area-entropy relation to derive Einstein equation

4 Entanglement Entropy Classical mechanics: definite state certain outcome for any measurement Quantum mechanics: definite state uncertain outcomes for some measurements Example: "i measurement of S z definitely gives ~ measurement of S x gives ~ 1 or with equal probability 2 ~ When only certain kinds of measurements are allowed, a definite (pure) state will effectively be indefinite (mixed) Suppose a system has two parts, but we can only measure one part Spin singlet state: Bi = p 1 ( "i #i #i "i) S B =0 2 To see that this is a pure state (superposition, not mixture, of "i #i and #i "i) requires access to both and B For an observer who only sees, effective state is mixed: B = 1 2 ( "ih" + #ih# ) S =ln2 (Classically, if whole is in a definite state then each part is also: S apple S B )

5 Entanglement Entropy In general: if ρ is state of full system, then effective state for subsystem is =Tr c Entanglement entropy is defined as von Neumann entropy of subsystem: S = Tr ln Not necessarily due only to entanglement (for example, in thermal state, S includes thermal entropy) Obeys many important properties, such as: Subadditivity: S B apple S + S B Strong subadditivity: (Lieb-Ruskai 73) S B + S BC S B + S BC B C

6 Entanglement Entropy in QFT In quantum field theories (& many-body systems), spatial regions are highly entangled with each other Consider microwave cavity Even in ground state, electromagnetic field fluctuates: zero-point quantum fluctuations of modes Each mode is distributed in space => fluctuations are spatially correlated => any part of cavity is entangled with rest

7 Entanglement Entropy in QFT In quantum field theories (& many-body systems), spatial regions are highly entangled with each other S depends on: parameters of theory state size and shape of region S is ultraviolet divergent due to entanglement of short-wavelength modes Finite pieces contain physically meaningful information Examples: Critical (conformal) theory in : (Holzhey-Larsen-Wilczek 94; Calabrese-Cardy 03) d =2 Gapped theory in : d =1 length(@) central charge S = L S = c 3 ln L t finite temperature, also extensive term: s(t)volume() L correlation length S = area(@) d 1 + L short-distance cutoff topological entanglement entropy (Kitaev-Preskill 05; Levin-Wen 05)

8 Entanglement Entropy in QFT In quantum field theories (& many-body systems), spatial regions are highly entangled with each other S Entropy depends on: parameters of theory state size and shape of region Powerful new way to think about QFTs and many-body systems: quantum criticality topological order renormalization-group flows energy conditions many-body localization quenches much more In general, difficult to compute even in free theories Simplifies in certain theories with many strongly-interacting fields

9 N SU(n) Consider a QFT with for example N Holographic dualities interacting fields Yang-Mills theory, N n 2 When is large, these fields may admit a collective description in terms of a small number of degrees of freedom classical (think of hydrodynamics) usually complicated However, in certain cases, when the fields are very strongly interacting, it simplifies dramatically: General relativity in d + 1 dimensions with cosmological constant Λ < 0, coupled to a small number of matter fields, subject to certain boundary conditions universe in a box (Maldacena 97)

10 Holographic dualities If QFT is conformal (scale-invariant), ground state is anti-de Sitter (ds) spacetime: ds radius d dimensions of QFT ds 2 = R2 z 2 dt 2 + dz 2 + d~x 2 extra dimension z = boundary of ds, where field theory lives ~x z Map between boundary and bulk is non-local If QFT is gapped (confining), space ends on wall at z max (correlation length) Many specific examples known in various dimensions (mostly supersymmetric, derived from string theory)

11 Holographic Dualities QFT N thermodynamic limit N!1 statistical fluctuations collective modes deconfined plasma S / N ds radius GR R d 1 G N ~ classical limit ~! 0 quantum fluctuations gravitational waves, etc. black hole S = area(horizon) 4G N ~ Planck area Holographic dualities are useful for computing many things in strongly interacting QFTs Let s talk about entanglement entropies... horizon

12 Holographic Entanglement Entropy Ryu-Takayanagi 06: S = area(m ) 4G N ~ / N m = minimal surface anchored z ~x Democratizes Bekenstein-Hawking Entanglement = geometry

13 Holographic Entanglement Entropy Ryu-Takayanagi 06: S = area(m ) 4G N ~ Geometrizes entanglement: m = minimal surface anchored z ~x rea-law UV divergence due to infinite area of near boundary m d =1 Conformal theory in : S = c 3 ln L m Gapped theory: wall imposes IR cutoff on entanglement (Klebanov, Kutasov, Murugan 07) Finite temperature: minimal surface hugs horizon => extensive entropy s(t)volume() m m wall horizon

14 Holographic Entanglement Entropy Quantum information theory is built into spacetime geometry Example: Strong subadditivity S B + S BC S BC + S B B C B C B C S B + S BC = = = S BC + S B (MH-Takayanagi 07) In fact, RT formula obeys all general properties of entanglement entropies (Hayden-MH-Maloney 11; MH 13) lso has special properties, such as phase transitions (MH 10) B B m B m B S B = S + S B S B <S + S B

15 Holographic Entanglement Entropy Where are the bits? (MH-Freedman 16) Rewrite RT formula, using max flow-min cut theorem S = max # of bit threads leaving Each bit thread has cross section of 4 Planck areas Represents entangled pair of qubits between and complement, or mixed qubit of horizon Clarifies how bits are distributed among different regions (conditional entropies, mutual informations, etc.)

16 Holographic Entanglement Entropy Many other issues: Entanglement entropies in specific systems General properties Derivation Quantum (1/N) corrections Time dependence... The big one: Does space emerge from entanglement? From bit threads?

17 Holographic Entanglement Entropy Many other issues: Entanglement entropies in specific systems General properties Derivation Quantum (1/N) corrections Time dependence... The big one: Does space emerge from entanglement? From bit threads?

18

19

20 Classical and Quantum Gravity General relativity: Gravity is a manifestation of the curvature of spacetime Geometry of spacetime (metric g µ ) is dynamical Einstein equation: G µ =8 G N T µ g µ Classical theory. curvature matter cosmological constant We know of many quantum theories of gravity (from string theory,... ). t long distances (compared to Planck length), they reduce to GR. They have various numbers of dimensions types of matter fields values of Unfortunately, we don t understand them well enough to directly answer the above questions.

21 Holographic Dualities Suppose we have a quantum theory of gravity in d +1 dimensions ( d =2, 3,... ). = 1 R 2 R l P 1 Simplest solution to Einstein equation is anti-de Sitter (ds) spacetime. No matter ( T µ =0). Space is hyperbolic (Lobachevsky) space. Boundary is infinitely far away, with infinite potential wall. Light can reach boundary (and reflect back) in finite time. quantum gravity hyperbolic space Let spacetime geometry fluctuate, fixing boundary conditions at infinity. Closed quantum system.

22 Holographic Dualities Maldacena 97: Quantum gravity in d +1dimensions with ds boundary conditions = d dimensional ordinary quantum field theory (without gravity). QFT lives on the boundary. Map between the two theories is non-local. quantum gravity QFT has a large number of strongly interacting fields: N = R l P d 1 = Rd 1 G N ~ 1 QFT

23 This helps to understand black hole entropy. But mysteries remain. Nothing special happens at a black hole horizon. What about other surfaces? Can their areas represent entropies? re there entropies that are intrinsic to a system --- not thermal?

24 Holographic Entanglement Entropy Black hole = thermal state Maldacena 01: 2 black holes joined by Einstein-Rosen bridge = 2 entangled QFTs S = a 4G N ~ B Ryu, Takayanagi 06 proposed that, in general, S = a 4G N ~ area of minimal surface between and B B Entanglement is the fabric of spacetime Simple & beautiful... widely applied... but is it right?

25 Holographic Entanglement Entropy MH 10: Explained how to apply replica trick to holographic theories. Debunked previous derivation of holographic formula. Showed that holographic formula predicts phase transition for separated regions. Confirmed using Euclidean quantum gravity & orbifold CFT techniques. Lewkowycz, Maldacena 13: General derivation of holographic formula. B B S B = S + S B S B <S + S B

26 Time-Dependent Holographic Entanglement Entropy What about time? Original (Ryu-Takayanagi) holographic formula assumes state is static. Hubeny, Rangamani, Takayanagi 07: For non-static states, replace minimal surface in bulk space with extremal surface in bulk spacetime. Simple & beautiful... widely applied... but is it right? Callan, He, MH 12: Obeys strong subadditivity in examples. Extremal surface goes behind horizons! MH, Hubeny, Lawrence, Rangamani 14: Nonetheless obeys causality. Implies that QFT state is encoded by (part of) spacetime behind horizon. MH, Myers, Wien 14: Proved that area of a general surface (not just extremal) is given by differential entropy in QFT.

27 Entanglement entropy in holographic theories: Enormous progress in recent years. Still many mysteries. Suggests a deep and general connection between entanglement and the geometry of spacetime. (How) does spacetime itself emerge from quantum mechanics? Stay tuned... Summary

28 Entanglement entropy in holographic theories: Enormous progress in recent years. Still many mysteries. Suggests a deep and general connection between entanglement and the geometry of spacetime. (How) does spacetime itself emerge from quantum mechanics? Stay tuned... Summary