Black hole final state conspiracies

McInnes, Brett

doi:10.1016/j.nuclphysb.2008.08.007

Cited by 20 publications

(22 citation statements)

References 64 publications

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“…In fact, the probability density becomes zero exactly at the origin. This indicates that quantization can perhaps remove classical singularities from gravity, as argued from many different points of view [8,9,[21][22][23][24][25][26][27].…”

Section: Introductionmentioning

confidence: 94%

Nonlocal (but also nonsingular) physics at the last stages of gravitational collapse

Saini

Stojković

2014

Phys. Rev. D

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We study the end stages of gravitational collapse of the thin shell of matter in ingoing Eddington-Finkelstein coordinates. We use the functional Schrodinger formalism to capture quantum effects in the near singularity limit. We find that that the equations of motion which govern the behavior of the collapsing shell near the classical singularity become strongly non-local. This reinforces previous arguments that quantum gravity in the strong field regime might be non-local. We managed to solve the non-local equation of motion for the dust shell case, and found an explicit form of the wavefunction describing the collapsing shell. This wavefunction and the corresponding probability density are non-singular at the origin, thus indicating that quantization should be able to rid gravity of singularities, just as it was the case with the singular Coulomb potential.

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Section: Introductionmentioning

confidence: 94%

Nonlocal (but also nonsingular) physics at the last stages of gravitational collapse

Saini

Stojković

2014

Phys. Rev. D

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“…For related literature see e.g. [104][105][106][107][108]. However, in our present work we only wanted to emphasize that one should pay more attention to the role of the singularities, and whether they are truly removed in a quantum theory of gravity.…”

Section: 2]mentioning

confidence: 99%

Black hole remnants and the information loss paradox

2015

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Forty years after the discovery of Hawking radiation, its exact nature remains elusive. If Hawking radiation does not carry any information out from the ever shrinking black hole, it seems that unitarity is violated once the black hole completely evaporates. On the other hand, attempts to recover information via quantum entanglement lead to the firewall controversy. Amid the confusions, the possibility that black hole evaporation stops with a "remnant" has remained unpopular and is often dismissed due to some "undesired properties" of such an object. Nevertheless, as in any scientific debate, the pros and cons of any proposal must be carefully scrutinized. We fill in the void of the literature by providing a timely review of various types of black hole remnants, and provide some new thoughts regarding the challenges that black hole remnants face in the context of the information loss paradox and its latest incarnation, namely the firewall controversy. The importance of understanding the role of curvature singularity is also emphasized, after all there remains a possibility that the singularity cannot be cured even by quantum gravity. In this context a black hole remnant conveniently serves as a cosmic censor. We conclude that a remnant remains a possible end state of Hawking evaporation, and if it contains large interior geometry, may help to ameliorate the information loss paradox and the firewall controversy. We hope that this will raise some interests in the community to investigate remnants more critically but also more thoroughly.

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“…[See also the discussion in [18] for an expression of the horizon area in terms of the dimensionless area Γ[L(p, 1)].] Thus in either case, for sufficiently large p, the black hole horizon is small.…”

Section: The Interiors Of Ads Black Lensesmentioning

confidence: 99%

Never judge a black hole by its area

Ong

2015

J. Cosmol. Astropart. Phys.

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Christodoulou and Rovelli have shown that black holes have large interiors that grow asymptotically linearly in advanced time, and speculated that this may be relevant to the information loss paradox. We show that there is no simple relation between the interior volume of an arbitrary black hole and its horizon area. That is, the volume enclosed is not necessarily a monotonically increasing function of the surface area. Black Holes and Their Large InteriorsAn asymptotically flat Schwarzschild black hole has a spherical event horizon. The usual metric of this geometry in 4-dimensions, in the units G = c = 1, iswhere M is the ADM mass, and r is the areal radius. That is, the area of the event horizon r h is the area of the 2-sphere: 4πr 2 h . Unlike its surface area, the concept of "the volume" of a black hole is a tricky one. The reason is that volume depends on the choice of 3-dimensional spacelike hypersurface. As such, no unique volume can be prescribed to a black hole. Furthermore, the interior of a static black hole is nevertheless dynamical, so one should definitely not think of a black hole as a black box that bounds a certain amount of volume that can be easily estimated from knowing the size of its area. This is well-known: a maximally extended Schwarzschild [Kruskal-Szekeres] geometry has an infinitely large asymptotically flat region on the "other side", connected via the Einstein-Rosen bridge. Similarly, one could attach a closed FLRW universe to the interior of a black hole via the Einstein-Rosen bridge, resulting in the socalled Wheeler's "bag-of-gold" geometry [1]. Even non-black hole configurations can have arbitrarily large interiors than their areas might suggest [2]. What about black holes that were formed from gravitational collapse and have no second asymptotic region?One important motivation to study the interiors of generic black holes is of course the information loss paradox. As matter falls into a black hole and the black hole gradually Hawking evaporates away, it seems that when the black hole disappears, the information of the in-fallen matter will be lost forever, thereby threatening the unitarity of quantum

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Black hole final state conspiracies

Cited by 20 publications

References 64 publications

Nonlocal (but also nonsingular) physics at the last stages of gravitational collapse

Nonlocal (but also nonsingular) physics at the last stages of gravitational collapse

Black hole remnants and the information loss paradox

Never judge a black hole by its area

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