Excluding black hole firewalls with extreme cosmic censorship

Page, Don N.

doi:10.1088/1475-7516/2014/06/051

Cited by 40 publications

(41 citation statements)

References 165 publications

(186 reference statements)

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“…Recently, a modern interpretation of the information-loss paradox, known as the "firewall" problem [25] (also see [9-11, 26, 27] for earlier versions and [28][29][30][31][32][33][34][35][36][37][38][39][40][41][42][43][44][45] for a sample of the related literature). We find the current analysis to be an essential step toward a resolution of this puzzle, but defer this discussion to future publications [46,47].…”

Section: Jhep02(2014)116mentioning

confidence: 99%

Phases of information release during black hole evaporation

Brustein

Medved

2014

J. High Energ. Phys.

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In a recent article, we have shown how quantum fluctuations of the background geometry modify Hawking's density matrix for black hole (BH) radiation. Hawking's diagonal matrix picks up small off-diagonal elements whose influence becomes larger with the number of emitted particles. We have calculated the "time-of-first-bit", when the first bit of information comes out of the BH, and the "transparency time", when the rate of information release becomes order unity. We have found that the transparency time is equal to the "Page time", when the BH has lost half of its initial entropy to the radiation, in agreement with Page's results. Here, we improve our previous calculation by keeping track of the time of emission of the Hawking particles and their back-reaction on the BH. Our analysis reveals a new time scale, the radiation "coherence time", which is equal to the geometric mean of the evaporation time and the light crossing time. We find, as for our previous treatment, that the time-of-first-bit is equal to the coherence time, which is much shorter than the Page time. But the transparency time is now much later than the Page time, just one coherence time before the end of evaporation. Close to the end, when the BH is parametrically of Planckian dimensions but still large, the coherence time becomes parametrically equal to the evaporation time, thus allowing the radiation to purify. We also determine the time dependence of the entanglement entropy of the early and late-emitted radiation. This entropy is small during most of the lifetime of the BH, but our qualitative analysis suggests that it becomes parametrically maximal near the end of evaporation.

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Section: Jhep02(2014)116mentioning

confidence: 99%

Phases of information release during black hole evaporation

Brustein

Medved

2014

J. High Energ. Phys.

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“…This is what one might have expected from the gravitational firewall debate [1][2][3][4][5][6][7][8][9][10][11]. However, if Alice crosses the firewall shortly before turning her detector off, the effect is the opposite: in this case the firewall helps Alice and Bob maintain their entanglement.…”

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confidence: 90%

“…The absence of cataclysmic events should continue to hold for young black hole firewalls. A firewall's prospective ability to resolve the information paradox must hence hinge on its detailed gravitational structure, presently poorly understood.Introduction.-If black hole evaporation preserves unitarity, it has been argued from preservation of correlations that the horizon of a shrinking black hole must develop a singularity even when the evaporation is still slow and the black hole remains macroscopic [1-3] (for a selection of debate and reviews see [4][5][6][7][8][9][10][11]). Modeling the gravitational aspects of this proposed singularity has remained elusive.…”

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confidence: 99%

(1+1)DCalculation Provides Evidence that Quantum Entanglement Survives a Firewall

Martín-Martínez

Louko

2015

Phys. Rev. Lett.

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We analyze how pre-existing entanglement between two Unruh-DeWitt particle detectors evolves when one of the detectors falls through a Rindler firewall in (1+1)-dimensional Minkowski space. The firewall effect is minor and does not wash out the detector-detector entanglement, in some regimes even preserving the entanglement better than Minkowski vacuum. The absence of cataclysmic events should continue to hold for young black hole firewalls. A firewall's prospective ability to resolve the information paradox must hence hinge on its detailed gravitational structure, presently poorly understood.Introduction.-If black hole evaporation preserves unitarity, it has been argued from preservation of correlations that the horizon of a shrinking black hole must develop a singularity even when the evaporation is still slow and the black hole remains macroscopic [1-3] (for a selection of debate and reviews see [4][5][6][7][8][9][10][11]). Modeling the gravitational aspects of this proposed singularity has remained elusive. For instance, the emergence of a Planck scale shell near the horizon of an astrophysical black hole seems to be in tension with the gravitational dynamics predicted by general relativity [12]. Nevertheless, the nongravitational aspects of the "firewall" version of the singularity [3] can be modeled with a quantum field in Minkowski spacetime: a state in which correlations across a Rindler horizon are severed can be written down by hand [13], mimicking the severing that the firewall argument of [3] posits to develop dynamically during black hole evaporation. This severing of correlations has strong similarities to that which ensues on the sudden insertion of a reflective wall in a spacetime [14,15]. The Rindler firewall state can be studied by usual quantum field theory techniques, and the conclusions should apply to young gravitational firewalls where the backreaction on the metric is still small.

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“…What we mean here is that geometries with trivial topology, i.e. with no-horizon, would dominate the path integral over the classical saddle points at large time 5 , as already suggested in [21] and [22] (see [23,24] for later discussions related to the firewall problem). Note that going away from the semiclassical limit, the dominant contribution to the correlation functions seems not to belong to the leading (Euclidean) saddle point approximation [7,21]; we will make this more clear later on.…”

Section: Introductionmentioning

confidence: 98%

Firewalls as artefacts of inconsistent truncations of quantum geometries

Germani

Sarkar

2015

Fortschritte der Physik

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In this paper we argue that a firewall is simply a manifestation of an inconsistent truncation of non-perturbative effects that unitarize the semiclassical black hole. Namely, we show that a naive truncation of quantum corrections to the Hawking spectrum at order ${\cal O}(e^{-S})$, inexorably leads to a "localised'' divergent energy density near the black hole horizon. Nevertheless, in the same approximation, a distant observer only sees a discretised spectrum and concludes that unitarity is achieved by ${\cal O}(e^{-S})$ effects. This is due to the fact that instead, the correct quantum corrections to the Hawking spectrum go like ${\cal O}( g^{tt} e^{-S})$. Therefore, while at a distance far away from the horizon, where $g^{tt}\approx 1$, quantum corrections {\it are} perturbative, they {\it do} diverge close to the horizon, where $g^{tt}\rightarrow \infty$. Nevertheless, these "corrections" nicely re-sum so that correlations functions are smooth at the would-be black hole horizon. Thus, we conclude that the appearance of firewalls is just a signal of the breaking of the semiclassical approximation at the Page time, even for large black holes.Comment: v4: explanation about the failure of the saddle point approximation and general clarifications adde

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Excluding black hole firewalls with extreme cosmic censorship

Cited by 40 publications

References 165 publications

Phases of information release during black hole evaporation

Phases of information release during black hole evaporation

(1+1)DCalculation Provides Evidence that Quantum Entanglement Survives a Firewall

Firewalls as artefacts of inconsistent truncations of quantum geometries

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