The Information Recovery Problem

Baccetti, Valentina; Husain, Viqar; Terno, Daniel R.

doi:10.3390/e19010017

Cited by 13 publications

(18 citation statements)

References 66 publications

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“…Approaches endeavouring to preserve unitary dynamics that are based on the analysis of matter alone require both an horizon and a singularity and so are not applicable as well. Indeed, our results strengthen the point of view that fully quantized joint gravity-matter dynamics must have uni-tary time evolution, particularly for systems that have a well-defined classical Hamiltonian, and so there cannot be any overall information loss [8,26,27]. The information loss paradox then goes the way other quantum paradoxes.…”

supporting

confidence: 74%

Do event horizons exist?

Baccetti

Mann

Terno

2017

Int. J. Mod. Phys. D

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Event horizons are the defining feature of classical black holes. They are the key ingredient of the information loss paradox which, as paradoxes in quantum foundations, is built on a combination of predictions of quantum theory and counterfactual classical features: neither horizon formation nor its crossing by a test body is observable. Furthermore, horizons are unnecessary for the production of Hawking-like radiation. We demonstrate that when this radiation is taken into account it prevents horizon crossing/formation in a large class of models. We conjecture that horizon avoidance is a general feature of collapse. The non-existence of event horizons dispels the paradox, but opens up important questions about thermodynamic properties of the resulting objects and correlations between different degrees of freedom.Comment: Honorable Mention in the 2017 Gravity Research Foundation Essay Competitio

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supporting

confidence: 74%

Do event horizons exist?

Baccetti

Mann

Terno

2017

Int. J. Mod. Phys. D

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“…Hence she does not see the vacuum, which is one of the elements in the chain of arguments at least in some versions of the firewall paradox [8]. Moreover, if the flux of energetic particles is desired to disentangle the early and late modes of emitted radiation, it has to not only avoid being a universal disentangler (forbidden by unitarity) [32], but also be weak enough so as to not destroy the horizon while being energetic enough for the erasure of information (at or above the Landauer bound) [33]. This is a highly nontrivial requirement.…”

Section: Discussionmentioning

confidence: 99%

Energy-momentum tensor and metric near the Schwarzschild sphere

et al. 2019

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Regularity of the horizon radius rg of a collapsing body constrains a limiting form of a spherically symmetric energy-momentum tensor near it. Its nonzero limit belongs to one of four classes that are distinguished only by two signs. As a result, close to rg the geometry can always be described by either an ingoing or outgoing Vaidya metric with increasing or decreasing mass. If according to a distant outside observer the trapped regions form in finite time, then the Einstein equations imply violation of the null energy condition. In this case the horizon radius and its rate of change determine the metric in its vicinity, and the hypersurface r = rg(t) is timelike during both the expansion and contraction of the trapped region. We present the implications of these results for the firewall paradox and discuss arguments that the required violation of the null energy condition is incompatible with the standard analysis of black hole evaporation.

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“…The sign of c w − a w depends on the kind of field [25]. For example, it is positive for a massless scalar field, and it is negative for a massless vector field 16 . When c w − a w > 0, (67) indicates that the outgoing radiation increases by the amount 3h(c w −a w ) 10 1 a(U) 2 as it goes to infinity from the surface.…”

Section: The Evaporating Black Holementioning

confidence: 99%

“…We start with examining the boundary condition. See the right of 16 However, > 0 holds for any kind of massless fields [25], and T UU is always positive at infinity. Here, the boundary condition (63) plays an important role.…”

Section: The Stationary Black Holementioning

confidence: 99%

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A Model of Black Hole Evaporation and 4D Weyl Anomaly

Kawai

Yokokura

2017

Universe

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Abstract:We analyze the time evolution of a spherically-symmetric collapsing matter from the point of view that black holes evaporate by nature. We consider conformal matters and solve the semi-classical Einstein equation G µν = 8πG T µν by using the four-dimensional Weyl anomaly with a large c coefficient. Here, T µν contains the contribution from both the collapsing matter and Hawking radiation. The solution indicates that the collapsing matter forms a dense object and evaporates without horizon or singularity, and it has a surface, but looks like an ordinary black hole from the outside. Any object we recognize as a black hole should be such an object.

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The Information Recovery Problem

Cited by 13 publications

References 66 publications

Do event horizons exist?

Do event horizons exist?

Energy-momentum tensor and metric near the Schwarzschild sphere

A Model of Black Hole Evaporation and 4D Weyl Anomaly

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