Black hole evaporation and semiclassical thin shell collapse

Valentina Baccetti, Sebastian Murk, Daniel R. Terno

Research output: Contribution to journalArticleResearchpeer-review

Abstract

In case of spherical symmetry, the assumptions of finite-time formation of a trapped region and regularity of its boundary—the apparent horizon—are sufficient to identify the form of the metric and energy-momentum tensor in its vicinity. By comparison with the known results for quasistatic evaporation of black holes, we complete the identification of their parameters. Consistency of the Einstein equations allows only two possible types of higher-order terms in the energy-momentum tensor. By using its local conservation, we provide a method of calculation of the higher-order terms, explicitly determining the leading-order regular corrections. Contraction of a spherically symmetric thin dust shell is the simplest model of gravitational collapse. Nevertheless, the inclusion of a collapse-triggered radiation in different extensions of this model leads to apparent contradictions. Using our results, we resolve these contradictions and show how gravitational collapse may be completed in finite time according to a distant observer.
LanguageEnglish
Article number064054
Number of pages11
JournalPhysical Review D
Volume100
Issue number6
DOIs
Publication statusPublished - 26 Sep 2019

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gravitational collapse
kinetic energy
evaporation
tensors
Einstein equations
regularity
contraction
horizon
conservation
dust
inclusions
symmetry
radiation

Cite this

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Black hole evaporation and semiclassical thin shell collapse. / Baccetti, Valentina; Murk, Sebastian; Terno, Daniel R.

In: Physical Review D, Vol. 100, No. 6, 064054, 26.09.2019.

Research output: Contribution to journalArticleResearchpeer-review

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