arXiv subjects

Bernard S. Kay

Publications and source records attributed to Bernard S. Kay.

34 records · Page 2Linked to original sources

arXiv2012

On the origin of thermality

It is well-known that a small system weakly coupled to a large energy bath in a total microcanonical ensemble will find itself in an (approximately) thermal state and, recently, it has been shown that, if the total state is, instead, a random pure state with energy in a narrow range, then the small system will still be approximately thermal with a high probability (wrt `Haar measure'). We ask what conditions are required for something resembling these 'traditional' and 'modern' thermality results to still hold when system and energy bath are of comparable size. In Part 1, we show that, for given system and energy-bath densities of states, s_S(e) and s_B(e), thermality does not hold in general, as we illustrate when both increase as powers of energy, but that it does hold in certain approximate senses, in both traditional and modern frameworks, when both grow as exp(be) or as exp(qe^2) and we calculate the system entropy in these cases. In their 'modern' version, our results rely on new quantities, which we introduce and call the S and B 'modapprox' density operators, which, we claim, will, with high probability, give a close approximation to the reduced density operator for the system and energy bath when the total state of system plus energy bath is a random pure state with energy in a narrow range. In Part 2 we clarify the meaning of these modapprox density operators and give arguments for our claim. The prime examples of non-small thermal systems are quantum black holes. Here and in two companion papers, we argue that current string-theoretic derivations of black hole entropy and thermal properties are incomplete and, on the question of information loss, inconclusive. However, we argue that these deficiencies are remedied with a modified scenario which relies on the modern strand of our methods and results here and is based on our previous 'matter-gravity entanglement hypothesis'.

cond-mat.stat-mech↗

arXiv2012

Modern foundations for thermodynamics and the stringy limit of black hole equilibria

We recall the existing string theory understanding of black hole entropy and argue it is incomplete but we put forward a modified version, based on the author's 'matter-gravity entanglement hypothesis', which, we claim, gives a more satisfactory understanding and also a resolution to the Information Loss Puzzle. This hypothesis pictures a black hole equilibrium as an, overall pure, state, with given energy, consisting of a black hole with its (mostly matter) atmosphere in a box and identifies the black hole's entropy with the pure state's matter-gravity entanglement entropy. We assume this equilibrium goes over, at weak string-coupling, to a pure state with similar energy consisting of a long string with a stringy atmosphere and that the matter-gravity entanglement entropy goes over to the entanglement entropy between (approximately) the long string and the stringy atmosphere. We also recall recent work (in a non-gravitational context) towards modern foundations for thermodynamics, where, in place of a total microcanonical ensemble, one assumes that a total system, consisting of a small (sub)system and an energy bath, is in a (random) pure state with energy in a given narrow range and shows that the small subsystem will then find itself in a thermal state. We present a new set of formulae, obtained in a companion paper, which generalize the setting of that work to cases where the system and energy bath are of comparable size. We apply these formulae to a model for our string equilibrium where the densities of states of the long string (replacing our energy bath) and stringy atmosphere (replacing our system) both grow exponentially. We find, for our picture of black hole equilibrium, a temperature of the order of the Hawking temperature and an entropy of the order of the Hawking entropy thus adding to the evidence for the viablity of our matter-gravity entanglement hypothesis.

gr-qc↗

arXiv2012

More about the stringy limit of black hole equilibria

We discuss further our proposed modification of the Susskind-Horowitz-Polchinski scenario in which black hole entropy goes over to string entropy as one scales the string length scale up and the string coupling constant down, keeping Newton's constant unchanged. In our approach, based on our 'matter-gravity entanglement hypothesis', 'string entropy' here should be interpreted as the likely entanglement entropy between (approximately) the single long string and the stringy atmosphere which, as we argue, arise in a pure multistring state of given energy in a (rescaled) box. In a previous simple analysis, we computed this entropy (with promising results) by assuming simple exponentially increasing densities of states for both long string and stringy atmosphere. Here, our starting point is a (more correct) density of states for each single string with the appropriate inverse-power prefactor and a low-energy cutoff. We outline how the relevant entanglement entropy should be calculated for this system and propose a plausible model, which draws on the work of Mitchell and Turok on the multi-string microcanonical ensemble, in which we adopt a similar density of states for long string and stringy atmosphere but now with cutoffs which scale with the total energy, E. With this scaling, we still find our entanglement entropy grows, in leading order, linearly with E and this translates to a black-hole entropy which goes as the square of the black-hole mass, thus retaining most of the promising features of our previous exponential-density-of-states model and providing further evidence for our matter-gravity entanglement hypothesis.

hep-th↗

arXiv2008

Pre-Holography

We construct a symplectic isomorphism, h, from classical Klein Gordon solutions of mass m on (d+1)-dimensional Lorentzian Anti de Sitter space (equipped with the usual symplectic form) to a certain symplectic space of functions on its conformal boundary (only) for all integer and half-integer Delta (= d/2 + (1/2)(d^2 + 4m^2)^{1/2}). h induces a large family of new examples of Rehren's algebraic holography in which the net of local quantum Klein Gordon algebras in AdS is seen to map to a suitably defined net of local algebras for the (generalized free) scalar conformal field with anomalous dimension Delta on d-dimensional Minkowski space (the AdS boundary). Relatedly, we show for these models that Bertola et al's boundary-limit holography becomes a quantum duality (only) if the test functions for boundary Wightman distributions are restricted in a particular way.

hep-th↗

arXiv2007

Expectation values, experimental predictions, events and entropy in quantum gravitationally decohered quantum mechanics

We restate Kay's 1998 hypothesis which simultaneously offers an objective definition for the entropy of a closed system, a microscopic foundation for the Second Law, a resolution of the Information Loss (and other) Black-Hole Puzzle(s) and an objective mechanism for decoherence. Presupposing a conventional unitary theory of low-energy quantum gravity, it offers all this by taking the physical density operator of a closed system to be the partial trace of its total density operator (assumed pure) over gravity and by defining its physical entropy to be its `matter-gravity entanglement entropy'. We also recall Kay's 1998 modified non-relativistic (many-body) quantum mechanics based on Kay's hypothesis with a Newtonian approximation to quantum gravity. In this modification, we find formal expectation values for certain `observables' such as momentum-squared and Parity are altered but those for functions of positions are unaltered. However, by arguing that every real measurement can ultimately be taken to be a position measurement, we prove that, in practice, it is impossible to detect any alteration at all and, in particular, we predict no alteration for Roger Penrose's experiment. Nevertheless, Kay's modification contains no Schrödinger Cat-like states, and also allows an `events' interpretation which we tentatively propose and begin to explore. We also obtain a Second-Law type result for a non-relativistic toy-model closed system and argue that similar results will apply for a wide class of model Newtonian and post-Newtonian closed systems although we argue that ordinary actual lab-sized systems can never be treated as closed for the purpose of calculating their entropy. Compared with `collapse models' such as GRW, Kay's Newtonian theory does a similar job while being free from ad hoc assumptions.

quant-ph↗

arXiv2007

Quantum field theory in curved spacetime

An encyclopedia article on mathematical aspects of quantum field theory in curved spacetime. Section titles are: Introduction and preliminaries; Construction of *-algebra for a real linear scalar field on globally hyperbolic spacetimes and some general theorems; Particle creation and the limitations of the particle concept; Theory of the stress-energy tensor; Hawking and Unruh effects; Non-globally hyperbolic spacetimes and the time-machine question; Other related topics and some warnings.

gr-qc↗

arXiv2006

The robustness of a many-body decoherence formula of Kay under changes in graininess and shape of the bodies

In ``Decoherence of macroscopic closed systems within Newtonian quantum gravity'' (Kay B S 1998 Class. Quantum Grav. 15 L89-L98) it was argued that, given a many-body Schroedinger wave function ψ(x_1,...,x_N) for the centre-of-mass degrees of freedom of a closed system of N identical uniform-mass balls of mass M and radius R, taking account of quantum gravitational effects and then tracing over the gravitational field amounts to multiplying the position-space density matrix ρ(x_1,...,x_N; x_1',...,x_N')= ψ(x_1,...,x_N)ψ*(x_1',...,x_N') by a multiplicative factor, which, if the positions {x_1,...,x_N; x_1',...,x_N'} are all much further away from one another than R, is well-approximated by the product from 1 to N over I, J, K (I 0) of radius r with centres at the vertices of a cubic lattice of spacing a (assumed to be very much bigger than 2r) and side 2La we establish the bound e^{-1/3}(r/a)^{1/n}La < R_eff < 2\sqrt 3(r/a)^{1/n} La.

gr-qc↗

arXiv2001

Application of linear hyperbolic PDE to linear quantum fields in curved spacetimes: especially black holes, time machines and a new semi-local vacuum concept

Several situations of physical importance may be modelled by linear quantum fields propagating in fixed spacetime-dependent classical background fields. For example, the quantum Dirac field in a strong and/or time-dependent external electromagnetic field accounts for the creation of electron-positron pairs out of the vacuum. Also, the theory of linear quantum fields propagating on a given background curved spacetime is the appropriate framework for the derivation of black-hole evaporation (Hawking effect) and for studying the question whether or not it is possible in principle to manufacture a time-machine. It is a well-established metatheorem that any question concerning such a linear quantum field may be reduced to a definite question concerning the corresponding classical field theory (i.e. linear hyperbolic PDE with non-constant coefficients describing the background in question) -- albeit not necessarily a question which would have arisen naturally in a purely classical context. The focus in this talk will be on the covariant Klein-Gordon equation in a fixed curved background, although we shall draw on analogies with other background field problems and with the time-dependent harmonic oscillator. The aim is to give a sketch-impression of the whole subject of Quantum Field Theory in Curved Spacetime, focussing on work with which the author has been personally involved, and also to mention some ideas and work-in-progress by the author and collaborators towards a new "semi-local" vacuum construction for this subject. A further aim is to introduce, and set into context, some recent advances in our understanding of the general structure of quantum fields in curved spacetimes which rely on classical results from microlocal analysis.

gr-qc↗

arXiv1998

Monotonicity with Volume of Entropy and of Mean Entropy for Translationally Invariant Systems as Consequences of Strong Subadditivity

We consider some questions concerning the monotonicity properties of entropy and mean entropy of states on translationally invariant systems (classical lattice, quantum lattice and quantum continuous). By taking the property of strong subadditivity, which for quantum systems was proven rather late in the historical development, as one of four primary axioms (the other three being simply positivity, subadditivity and translational invariance) we are able to obtain results, some new, some proved in a new way, which appear to complement in an interesting way results proved around thirty years ago on limiting mean entropy and related questions. In particular, we prove that as the sizes of boxes in Z^n or R^n increase in the sense of set inclusion, (1) their mean entropy decreases monotonically and (2) their entropy increases monotonically. Our proof of (2) uses the notion of "m-point correlation entropies" which we introduce and which generalize the notion of "index of correlation" (see e.g. R. Horodecki, Phys. Lett. A 187 p145 1994). We mention a number of further results and questions concerning monotonicity of mean entropy for more general shapes than boxes and for more general translationally invariant (/homogeneous) lattices and spaces than Z^n or R^n.

math-ph↗

arXiv1998

Decoherence of Macroscopic Closed Systems within Newtonian Quantum Gravity

A theory recently proposed by the author aims to explain decoherence and the thermodynamical behaviour of closed systems within a conservative, unitary, framework for quantum gravity by assuming that the operators tied to the gravitational degrees of freedom are unobservable and equating physical entropy with matter-gravity entanglement entropy. Here we obtain preliminary results on the extent of decoherence this theory predicts. We treat first a static state which, if one were to ignore quantum gravitational effects, would be a quantum superposition of two spatially displaced states of a single classically well describable ball of uniform mass density in empty space. Estimating the quantum gravitational effects on this system within a simple Newtonian approximation, we obtain formulae which predict e.g. that as long as the mass of the ball is considerably larger than the Planck mass, such a would-be-coherent static superposition will actually be decohered whenever the separation of the centres of mass of the two ball-states excedes a small fraction (which decreases as the mass of the ball increases) of the ball radius. We then obtain a formula for the quantum gravitational correction to the would-be-pure density matrix of a non-relativistic many-body Schroedinger wave function and argue that this formula predicts decoherence between configurations which differ (at least) in the "relocation" of a cluster of particles of Planck mass. We estimate the entropy of some simple model closed systems, finding a tendency for it to increase with "matter-clumping" suggestive of a link with existing phenomenological discussions of cosmological entropy increase.

hep-th↗

arXiv1998

Entropy Defined, Entropy Increase and Decoherence Understood, and Some Black-Hole Puzzles Solved

Statistical mechanics explains thermodynamics in terms of (quantum) mechanics by equating the entropy of a microstate of a closed system with the logarithm of the number of microstates in the macrostate to which it belongs, but the question `what is a macrostate?' has never been answered except in a vague, subjective, way. However Hawking's discovery of black hole evaporation led to a formula for black hole entropy with no subjective element. In this letter, we argue from this result, together with the assumption that `black hole thermodynamics is just ordinary thermodynamics applied to black holes', that a macrostate for a general (quantum gravitational) closed system is an equivalence class of matter-gravity microstates with the same expectation values for the matter degrees of freedom alone. Not only does this finally answer the question `what is entropy?', but it also predicts the equality of the thermodynamic entropy of a black hole with the matter and the gravity entropy-like quantities derived from the Euclidean path integral. Furthermore it gives us a clear glimpse of an ultimate synthesis of quantum theory and gravity in which we see that (a) gravity acts as a universal environment, thus predicting that, if the initial state of the universe is unentangled, its entropy must go on increasing forever, (b) the gravitational field has degrees of freedom, but no observables, thus enabling gravity to perform the trick of providing an objective continual process of decoherence. All the above rests on the validity of unitarity. The `information-loss puzzle' had raised doubts about that. But we suggest a resolution for this puzzle.

hep-th↗

arXiv1997

The thermal and two-particle stress-energy must be ill-defined on the 2-d Misner space chronology horizon

We show that an analogue of the (four dimensional) image sum method can be used to reproduce the results, due to Krasnikov, that for the model of a real massless scalar field on the initial globally hyperbolic region IGH of two-dimensional Misner space there exist two-particle and thermal Hadamard states (built on the conformal vacuum) such that the (expectation value of the renormalised) stress-energy tensor in these states vanishes on IGH. However, we shall prove that the conclusions of a general theorem by Kay, Radzikowski and Wald still apply for these states. That is, in any of these states, for any point b on the Cauchy horizon and any neighbourhood N of b, there exists at least one pair of non-null related points (x,x'), with x and x' in the intersection of IGH with N, such that (a suitably differentiated form of) its two-point function is singular. (We prove this by showing that the two-point functions of these states share the same singularities as the conformal vacuum on which they are built.) In other words, the stress-energy tensor in any of these states is necessarily ill-defined on the Cauchy horizon.

gr-qc↗

arXiv1997

Quantum Field Theory on Spacetimes with a Compactly Generated Cauchy Horizon

We prove two theorems which concern difficulties in the formulation of the quantum theory of a linear scalar field on a spacetime, (M,g_{ab}), with a compactly generated Cauchy horizon. These theorems demonstrate the breakdown of the theory at certain `base points' of the Cauchy horizon, which are defined as `past terminal accumulation points' of the horizon generators. Thus, the theorems may be interpreted as giving support to Hawking's `Chronology Protection Conjecture', according to which the laws of physics prevent one from manufacturing a `time machine'. Specifically, we prove: Theorem 1: There is no extension to (M,g_{ab}) of the usual field algebra on the initial globally hyperbolic region which satisfies the condition of F-locality at any base point. In other words, any extension of the field algebra must, in any globally hyperbolic neighbourhood of any base point, differ from the algebra one would define on that neighbourhood according to the rules for globally hyperbolic spacetimes. Theorem 2: The two-point distribution for any Hadamard state defined on the initial globally hyperbolic region must (when extended to a distributional bisolution of the covariant Klein-Gordon equation on the full spacetime) be singular at every base point x in the sense that the difference between this two point distribution and a local Hadamard distribution cannot be given by a bounded function in any neighbourhood (in MXM) of (x,x). Theorem 2 implies quantities such as the renormalized expectation value of ϕ^2 or of the stress-energy tensor are necessarily ill-defined or singular at any base point. The proofs rely on the `Propagation of Singularities' theorems of Duistermaat and Hörmander.

gr-qc↗

arXiv1997

Quantum Fields in Curved Spacetime: Non Global Hyperbolicity and Locality

We briefly review the current status of the algebraic approach to quantum field theory on globally hyperbolic spacetimes, both axiomatic -- for general field theories, and constructive -- for a linear Klein-Gordon model. We recall the concept of F-locality, introduced in the latter context in BS Kay: Rev. Math. Phys., Special Issue, 167-195 (1992) and explain how it can be formulated at an axiomatic level for a general field theory (as a condition on algebras-with-net-structure) on both globally hyperbolic and non globally hyperbolic spacetimes. We also discuss the current status of the question whether/when algebras satisfying F-locality can exist for the Klein-Gordon model on spacetimes which are chronology violating.

gr-qc↗

arXiv1996

Stress-Energy Must be Singular on the Misner Space Horizon even for Automorphic Fields

We use the image sum method to reproduce Sushkov's result that for a massless automorphic field on the initial globally hyperbolic region $IGH$ of Misner space, one can always find a special value of the automorphic parameter $α$ such that the renormalized expectation value $\langleα|T_{ab}|α\rangle$ in the {\it Sushkov state} ``$\langleα|\cdot|α\rangle$'' (i.e. the automorphic generalization of the Hiscock-Konkowski state) vanishes. However, we shall prove by elementary methods that the conclusions of a recent general theorem of Kay-Radzikowski-Wald apply in this case. I.e. for any value of $α$ and any neighbourhood $N$ of any point $b$ on the chronology horizon there exists at least one pair of non-null related points $(x,x') \in (N\cap IGH)\times (N\cap IGH)$ such that the renormalized two-point function of an automorphic field $G^α_{\rm ren}(x,x')$ in the Sushkov state is singular. In consequence $\langleα|T_{ab}|α\rangle$ (as well as other renormalized expectation values such as $\langleα|ϕ^2|α\rangle$) is necessarily singular {\it on} the chronology horizon. We point out that a similar situation (i.e. singularity {\it on} the chronology horizon) holds for states on Gott space and Grant space.

gr-qc↗

arXiv1995

Long Range Effects of Cosmic String Structure

We combine and further develop ideas and techniques of Allen \& Ottewill, Phys. Rev.D, {\bf 42}, 2669 (1990) and Kay \& Studer Commun. Math. Phys., {\bf 139}, 103 (1991) for calculating the long range effects of cosmic string cores on classical and quantum field quantities far from an (infinitely long, straight) cosmic string. We find analytical approximations for (a) the gravity-induced ground state renormalized expectation values of $\hatφ^2$ and $\hat T_μ^ν$ for a non-minimally coupled quantum scalar field far from a cosmic string (b) the classical electrostatic self force on a test charge far from a superconducting cosmic string. Surprisingly -- even at cosmologically large distances -- all these quantities would be very badly approximated by idealizing the string as having zero thickness and imposing regular boundary conditions; instead they are well approximated by suitably fitted strengths of logarithmic divergence at the string core. Our formula for ${\langle {\hat φ}^2 \rangle}$ reproduces (with much less effort and much more generality) the earlier numerical results of Allen \& Ottewill. Both ${\langle {\hat φ}^2 \rangle}$ and ${\langle {\hat T}_μ{}^ν \rangle}$ turn out to be ``weak field topological invariants'' depending on the details of the string core only through the minimal coupling parameter ``$ξ$'' (and the deficit angle). Our formula for the self-force (leaving aside relatively tiny gravitational corrections) turns out to be attractive: We obtain, for the self-potential of a test charge $Q$ a distance $r$ from a (GUT scale) superconducting string, the formula $- Q^2/(16ε_0r\ln(qr))$ where $q$ is an (in principle, computable) constant of the order of the inverse string radius.

gr-qc↗