Quantum radiation from a sandwich black hole

Frolov, Valeri P.; Zelnikov, Andrei

doi:10.1103/physrevd.95.044042

Cited by 19 publications

(38 citation statements)

References 65 publications

(91 reference statements)

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“…Then several papers followed. A non exhaustive list of papers is [8] [9] [10] [6] [12] [13] [14][15] [16] [17] [18] [19] [20] [21] [22] [23]. For a review, see [24].…”

Section: Introductionmentioning

confidence: 99%

A note on singular and non-singular black holes

Chinaglia

Zerbini

2017

Gen Relativ Gravit

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An attempt is made in order to clarify the so called regular black holes issue. It is revisited that if one works within General Relativity minimally coupled with non linear source, mainly of electromagnetic origin, and within a static spherically symmetric ansatz for the metric, there is still room for singular contribution to the black hole solution. A reconstruction method is proposed and several examples are discussed, including new ones. A possible way to obtain a non singular black hole is introduced, and in this case, several known examples are re-discussed, and new ones are provided.Comment: 15 pages, version to appear in GRG, references adde

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“…Then several papers followed. A non exhaustive list of papers is [8] [9] [10] [6] [12] [13] [14][15] [16] [17] [18] [19] [20] [21] [22] [23]. For a review, see [24].…”

Section: Introductionmentioning

confidence: 99%

A note on singular and non-singular black holes

Chinaglia

Zerbini

2017

Gen Relativ Gravit

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“…In particular, for example, the model presented here suggests an improvement to the recent interesting calculation by Frolov and Zelnikov, who have studied the quantum radiation from an evaporating modified Hayward metric [45,46]. They found, in addition to the Hawking radiation, an unwanted burst of radiation emanating from the inner horizon.…”

Section: Towards a Self-consistent Evaporation Modelmentioning

confidence: 58%

“…Significant attention has been given recently to the question of self-consistent BH evaporation models (related examples include [42][43][44][45][46]). Typically the idea is to postulate an evaporating BH spacetime, treat it as a fixed background for a quantum field theory, and show that a renormalized stress tensor for the field theory matches the background curvature -or at least find some evidence that the field theory and background are compatible.…”

Section: Towards a Self-consistent Evaporation Modelmentioning

confidence: 99%

See 1 more Smart Citation

Understanding black hole evaporation using explicitly computed Penrose diagrams

Schindler¹,

Aguirre²,

Kuttner³

2020

Phys. Rev. D

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Rigorously computed Penrose diagrams are plotted for a semiclassical model of black hole formation and evaporation, in which black holes form by the accretion of infalling spherical shells of matter and subsequently evaporate by emitting spherical shells of Hawking radiation. The method allows arbitrary interior solutions of the form ds 2 = −f (r) dt 2 +f (r) −1 dr 2 +r 2 dΩ 2 , including singular and nonsingular models. Matter dynamics are visualized by explicitly plotting proper densities and pressures in the diagrams, as well as by tracking the location of trapped surfaces and energy condition violations. The most illustrative model accurately approximates the standard time evolution for black hole thermal evaporation; its time dependence and causal structure are analyzed by inspection of the rigorous diagram. The resulting insights contradict some common intuitions and assumptions, and we point out some examples in the literature with assumptions that do not hold up in our more detailed model. Based on the new diagrams, we argue for an improved understanding of the Hawking radiation process, propose an improved definition of "black hole" in the presence of evaporation, and suggest some implications regarding information preservation and unitarity.

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“…There is a direct relation of this result with a well known phenomenon of mass inflation [30]. It was demonstrated in the paper [29] that this is a consequence of the large value of the (negative) surface gravity on the inner horizon, which in a standard models) is of the order of −1 . The surface gravity on the inner horizon can be suppressed by including a specially chosen redshift factor in the metric (see e.g.…”

Section: Introductionmentioning

confidence: 64%

Quantum radiation from an evaporating nonsingular black hole

Frolov

Zelnikov

2017

Phys. Rev. D

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In this paper we study quantum radiation from an evaporating spherically symmetric non-singular black hole. We used a modified Hayward metric for a description of a non-singular black hole interior. We assume that the mass parameter of this metric depends on the advanced time, and choose this dependence so that it properly reproduces both black hole formation and its subsequent evaporation. We consider a quantum massless scalar field propagating in this geometry and use 2D approximation for the calculation of the quantum average of the stress-energy tensor in the initial vacuum state. For the calculation of this quantity it is sufficient to find a map between the Killing times u+ and u− at the future and past null infinities, established by the propagation of the radial null rays. In this formalism the quantum energy flux at the future null infinity can be expressed in terms of the function u+(u−) and its derivatives up to the third order. We developed a special formalism, which allows one to reduce the problem of the calculation of the quantum energy flux and other observables to a solution of a simple set of ordinary differential equations. We used this approach to study quantum effects in two cases: i) with the trivial, α = 1 and ii) the non-trivial, α = 1, redshift function. We demonstrated, that in both cases there exists an outburst of the quantum energy radiation from the inner domain of the black hole, close to the inner part of its apparent horizon. For α = 1 this outburst is exponentially large. Its appearance is a direct consequence of the so-called mass inflation effect. We also demonstrated, that this severe problem can be solved by a proper choice of the redshift function. However, even in this case the emitted energy can be much larger than the initial mass of the evaporating black hole. This means that for a construction of a self-consistent model of a non-singular evaporating black hole the back-reaction effects are highly important.

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Quantum radiation from a sandwich black hole

Cited by 19 publications

References 65 publications

A note on singular and non-singular black holes

A note on singular and non-singular black holes

Understanding black hole evaporation using explicitly computed Penrose diagrams

Quantum radiation from an evaporating nonsingular black hole

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