Formation and evaporation of nonsingular black holes.

By S. Hayward. Physical Review Letters, 2005

773 citations recorded by the source corpus.

Regular (nonsingular) space-times are given that describe the formation of a (locally defined) black hole from an initial vacuum region, its quiescence as a static region, and its subsequent evaporation to a vacuum region. The static region is Bardeen-like, supported by finite density and pressures, vanishing rapidly at large radius and behaving as a cosmological constant at small radius. The dynamic regions are Vaidya-like, with ingoing radiation of positive-energy flux during collapse and negative-energy flux during evaporation, the latter balanced by outgoing radiation of positive-energy flux and a surface pressure at a pair creation surface. The black hole consists of a compact space-time region of trapped surfaces, with inner and outer boundaries that join circularly as a single smooth trapping horizon.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/78eec0cf486cddbd24819e0bb1b0b8cec909b9cd

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Citations in the corpus

Planck stars (2014, methodology): “In the presence of evaporation, the inner horizon grows, fed by the ingoing partners of the Hawking pairs [33] therefore α(t) increases while m(t) decreases.”
Black Hole Remnants and the Information Loss Paradox (2014, background): “, in the Vaidya approximation or numerical realization] [84].”
Constraints on black-hole charges with the 2017 EHT observations of M87* (2021, methodology): “2 the shadow areal radius rsh,A for a number of stationary black holes, such as Kerr [39], Kerr-Newman (KN) [40], Sen [41], and the rotating versions of the Bardeen and Hayward black holes [42].”
Spherical black holes with regular center: a review of existing models including a recent realization with Gaussian sources (2008, background): “See, for instance, [66] and the references discussed in section 3 for recent examples.”