The BTZ black hole violates strong cosmic censorship

Dias, Óscar J. C.; Reall, Harvey S.; Santos, Jorge E.

doi:10.1007/jhep12(2019)097

Cited by 75 publications

(162 citation statements)

References 67 publications

(189 reference statements)

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“…Hence, classically, the stress tensor becomes as regular as we wish across the Cauchy horizon, implying an even stronger violation of sCC than in the case of RNdS at the classical level. The authors [41] have also considered the expected quantum stress tensor in the Hartle-Hawking state and have presented arguments that it similarly becomes arbitrarily regular at the Cauchy horizon when we approach extremality, in marked contrast to our results in RNdS.…”

Section: Comparison With the Btz Black Holecontrasting

confidence: 83%

“…In sec. 6 we compare our results to the case of the BTZ black hole recently analyzed by [41], where, in fact, C = 0. In sec.…”

Section: Introductionmentioning

confidence: 85%

“…However, in contrast with RNdS, they showed that α is not the spectral gap (3) of all quasi-normal modes in region I, but only of the "counter-rotating" ones. As a consequence, it can be seen [41] that β → ∞ in the BTZ case as the spacetime approaches extremality r − → r + . Hence, classically, the stress tensor becomes as regular as we wish across the Cauchy horizon, implying an even stronger violation of sCC than in the case of RNdS at the classical level.…”

Section: Comparison With the Btz Black Holementioning

confidence: 93%

“…In [41] Dias et al have studied the stress tensor of a scalar field obeying ( − µ 2 )Φ = 0 in the 3-dimensional BTZ black hole spacetime [84,85]. In local coordinates it has the metric g = −f dt 2 + f −1 dr 2 + r 2 (dφ − Ωdt) 2 ,…”

Section: Comparison With the Btz Black Holementioning

confidence: 99%

“…and Penrose diagram as in Figure 11. (For simplicity, we have set the AdS radius L = 1; we refer to [41] for details on how to construct the diagram.) Even though the BTZ black hole is a solution with a negative cosmological constant, these authors showed that the regularity of the classical stress tensor T µν is governed by a parameter β similar to (2).…”

Section: Comparison With the Btz Black Holementioning

confidence: 99%

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Quantum instability of the Cauchy horizon in Reissner–Nordström–deSitter spacetime

Hollands

Wald

Zahn

2020

Class. Quantum Grav.

125

134

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In classical General Relativity, the values of fields on spacetime are uniquely determined by their values at an initial time within the domain of dependence of this initial data surface. However, it may occur that the spacetime under consideration extends beyond this domain of dependence, and fields, therefore, are not entirely determined by their initial data. This occurs, for example, in the well-known (maximally) extended Reissner-Nordström or Reissner-Nordström-deSitter (RNdS) spacetimes. The boundary of the region determined by the initial data is called the "Cauchy horizon." It is located inside the black hole in these spacetimes. The strong cosmic censorship conjecture asserts that the Cauchy horizon does not, in fact, exist in practice because the slightest perturbation (of the metric itself or the matter fields) will become singular there in a sufficiently catastrophic way that solutions cannot be extended beyond the Cauchy horizon. Thus, if strong cosmic censorship holds, the Cauchy horizon will be converted into a "final singularity," and determinism will hold. Recently, however, it has been found that, classically this is not the case in RNdS spacetimes in a certain range of mass, charge, and cosmological constant. In this paper, we consider a quantum scalar field in RNdS spacetime and show that quantum theory comes to the rescue of strong cosmic censorship. We find that for any state that is nonsingular (i.e., Hadamard) within the domain of dependence, the expected stress-tensor blows up with affine parameter, V , along a radial null geodesic transverse to the Cauchy horizon as T V V ∼ C/V 2 with C independent of the state and C = 0 generically in RNdS spacetimes. This divergence is stronger than in the classical theory and should be sufficient to convert the Cauchy horizon into a singularity through which the spacetime cannot be extended as a (weak) solution of the semiclassical Einstein equation. This behavior is expected to be quite general, although it is possible to have C = 0 in certain special cases, such as the BTZ black hole. arXiv:1912.06047v1 [gr-qc] 12 Dec 2019As we shall show in sec. 3, the behavior of the quantum stress tensor is determined by the trace anomaly and the continuity equation alone. We find that eq. (5) holds, with C ∼ κ 2 c − κ 2 − . Our arguments are technically rather 3 Our arguments rest on the assumption of regularity across the cosmological horizon, or the weaker condition that Tvv vanishes on the cosmological horizon, with v the "Killing parameter". This condition has a natural limit in RN, that of absence of radiation infalling from spatial infinity. It seems natural to discuss the behavior at the Cauchy horizon in terms of such asymptotic conditions, as without asymptotic conditions also the classical consideration of strong cosmic censorship becomes meaningless, as discussed for example in the Introduction to [12]: The domain of dependence of a compact achronal set in any globally hyperbolic spacetime has a Cauchy horizon, across which it is of course smoothly ex...

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Section: Comparison With the Btz Black Holecontrasting

confidence: 83%

“…In sec. 6 we compare our results to the case of the BTZ black hole recently analyzed by [41], where, in fact, C = 0. In sec.…”

Section: Introductionmentioning

confidence: 85%

Section: Comparison With the Btz Black Holementioning

confidence: 93%

Section: Comparison With the Btz Black Holementioning

confidence: 99%

Section: Comparison With the Btz Black Holementioning

confidence: 99%

See 3 more Smart Citations

Quantum instability of the Cauchy horizon in Reissner–Nordström–deSitter spacetime

Hollands

Wald

Zahn

2020

Class. Quantum Grav.

125

134

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Internal structure of hairy rotating black holes in three dimensions

Gao,

Liu,

Lyu

2024

J. High Energ. Phys.

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We construct hairy rotating black hole solutions in three dimensional Einstein gravity coupled to a complex scalar field. When we turn on a real and uniform source on the dual CFT, the black hole is stationary with two Killing vectors and we show that there is no inner horizon for the black hole and the system evolves smoothly into a Kasner universe. When we turn on a complex and periodic driving source on the dual CFT with a phase velocity equal to the angular velocity of the black hole, we have a time-dependent black hole with only one Killing vector. We show that inside the black hole, after a rapid collapse of the Einstein-Rosen bridge, oscillations of the scalar field follow. Then the system evolves into the Kasner epoch with possible Kasner inversion, which occurs in most of the parameter regimes. In both cases, one of the metric fields obeys a simple relation between its value at the horizon and in the Kasner epoch.

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Holography of time machines

Tomašević

2022

J. High Energ. Phys.

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We use holography to examine the response of interacting quantum fields to the appearance of closed timelike curves in a dynamically evolving background that initially does not contain them. For this purpose, we study a family of two-dimensional spacetimes that model very broad classes of wormhole time machines. The behavior of strongly coupled conformal theories in these spacetimes is then holographically described by three-dimensional AdS bulk geometries that we explicitly construct. The dual bulk spacetime is free from any divergences, but splits into two disconnected components, without and with CTCs, which are joined only through the boundary; then, passages across the chronology horizon are impossible for any field excitations. In dual terms, the strong self-interaction of the CFT decouples the pathological part from the rest of the spacetime. We also find that entangling the CFTs in two separate time machines connects them through a traversable bulk wormhole. Nevertheless, any entanglement-assisted chronology violations will be prevented by quantum bulk corrections, i.e., subleading 1/N effects, again without needing any gravitational backreaction of the CFT. We are led to speculate that chronology may be protected without involving Planck scale physics.

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The BTZ black hole violates strong cosmic censorship

Cited by 75 publications

References 67 publications

Quantum instability of the Cauchy horizon in Reissner–Nordström–deSitter spacetime

Quantum instability of the Cauchy horizon in Reissner–Nordström–deSitter spacetime

Internal structure of hairy rotating black holes in three dimensions

Holography of time machines

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