Quantum kicks near a Cauchy horizon

Juárez-Aubry, Benito A.; Louko, Jorma

doi:10.48550/arxiv.2109.14601

Cited by 2 publications

(2 citation statements)

References 38 publications

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“…In the limit m m c , the outer horizon is approximately the Schwarzschild radius r + ≈ 2M and the inner horizon is approximately r − ≈ l (this "core" is gravitationally repulsive since the geometry near the core is de Sitter). 7 We remark that the detector response calculations (or rather, transition rate calculations) for Reissner-Nordström black holes were recently investigated in order to understand the effect of Cauchy horizons on infalling detectors [50].…”

Section: Hayward Metricmentioning

confidence: 99%

Unruh-DeWitt detector in dimensionally-reduced static spherically symmetric spacetimes

Tjoa

Mann

2022

J. High Energ. Phys.

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We study the dynamics of an Unruh-DeWitt detector interacting with a massless scalar field in an arbitrary static spherically symmetric spacetimes whose metric is characterised by a single metric function f(r). In order to obtain clean physical insights, we employ the derivative coupling variant of the Unruh-DeWitt model in (1+1) dimensions where powerful conformal techniques enable closed-form expressions for the vacuum two-point functions. Due to the generality of the formalism, we will be able to study a very general class of static spherically symmetric (SSS) background. We pick three examples to illustrate our method: (1) non-singular Hayward black holes, (2) the recently discovered D → 4 limit of Gauss-Bonnet black holes, and (3) the “black bounce” metric that interpolates Schwarzschild black holes and traversable wormholes. We also show that the derivative coupling Wightman function associated with the generalized Hartle-Hawking vacuum satisfies the KMS property with the well-known temperature f′(rH)/(4π), where rH is the horizon radius.

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Section: Hayward Metricmentioning

confidence: 99%

Unruh-DeWitt detector in dimensionally-reduced static spherically symmetric spacetimes

Tjoa

Mann

2022

J. High Energ. Phys.

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“…In any case, in one or other of these variants, semiclassical gravity continues to be of great interest, and has been applied to problems or inspired studies in black hole physics [47,48,75,96,73], cosmology [12,15,19,22,43,57,72,84,85,86], cosmic censorship [10,11,18,23,53,54,55,60], quantum inequalities and singularity theorems [33,26,27,28,29,29,35,37], the ruling-out of faster-than-light communication and time travel [13,14,32,36,49,65,64], etc. Conceptual questions have been addressed in [75,68,81,93], while the mathematical structure of the theory has been studied e.g.…”

Section: Introductionmentioning

confidence: 99%

On the initial value problem for semiclassical gravity without and with quantum state collapses

Juárez-Aubry¹,

Kay²,

Miramontes³

et al. 2022

Preprint

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Semiclassical gravity is the theory in which the classical Einstein tensor of a spacetime is coupled to quantum matter fields propagating on the spacetime via the expectation value of their renormalized stress-energy tensor in a quantum state. We explore two issues, taking the Klein Gordon equation as our model quantum field theory. The first is the provision of a suitable initial value formulation for the theory. Towards this, we address the question, for given initial data consisting of the classical metric and its first three 'time' derivatives off the surface together with a choice of initial quantum state, of what is an appropriate 'surface Hadamard' condition such that, when the relevant constraint equations hold too, it is reasonable to conjecture that there will be a Cauchy development whose quantum state is Hadamard. This requires dealing with the fact, that given two points on an initial surface, the spacetime geodesic between them does not, in general, lie in that surface. So the geodesic distance that occurs in the Hadamard subtraction differs from the geodesic distance intrinsic to the initial surface. We handle this complication with a suitable 3dimensional covariant Taylor expansion. Moreover the renormalized expectation value of the stress-energy tensor in the initial surface depends explicitly on the fourth 'time' derivative of the metric, which is not part of the initial data, but which we argue is given, implicitly, by the semiclassical Einstein equations on the initial surface. We also introduce the notion of physical solutions, which, inspired by a 1993 proposal of Parker and Simon, we define to be solutions which are smooth in at = 0 -and conjecture that, for these, the second and third time derivatives of the metric will be determined by the remaining initial data. Finally we point out that a simpler treatment of the initial value problem can be had if we adopt yet more of the spirit of Parker and Simon and content ourselves with solutions to order which are Hadamard to order . A further simplification occurs if we consider semiclassical gravity to order 0 . This resembles classical general relativity in that it is free from the complications of higher derivative terms and does not require any Hadamard condition. But it can still incorporate nontrivial quantum features such as superpositions of classical-like quantum states of the matter fields. Our second issue concerns the prospects

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Quantum kicks near a Cauchy horizon

Cited by 2 publications

References 38 publications

Unruh-DeWitt detector in dimensionally-reduced static spherically symmetric spacetimes

Unruh-DeWitt detector in dimensionally-reduced static spherically symmetric spacetimes

On the initial value problem for semiclassical gravity without and with quantum state collapses

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