In spherical symmetry, solutions of the semiclassical Einstein equations belong to one of two possible classes. Both classes contain solutions that—depending on the dynamic behavior of the horizon—describe evaporating physical black holes or expanding white holes (trapped/anti-trapped regions that form in finite time of a distant observer). These solutions are real-valued only if the null energy condition (NEC) is violated in the vicinity of the Schwarzschild sphere. We review their properties and describe the only consistent black hole formation scenario. While the curvature scalars are finite on the outer apparent/anti-trapping horizon, it is still a weakly singular surface. This singularity manifests itself in a mild firewall. Near the inner apparent horizon, the NEC is satisfied. Models of static regular black holes are known to be unstable, but since dynamic models of regular black holes are severely constrained by self-consistency requirements, their stability requires further investigation.
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March 2022
Research Article|
March 08 2022
Semiclassical black holes and horizon singularities
Special Collection:
Celebrating Sir Roger Penrose's Nobel Prize
Pravin K. Dahal
;
Pravin K. Dahal
1
Department of Physics and Astronomy, Macquarie University
, Sydney, NSW 2109, Australia
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Sebastian Murk
;
Sebastian Murk
1
Department of Physics and Astronomy, Macquarie University
, Sydney, NSW 2109, Australia
2
Sydney Quantum Academy
, Sydney, NSW 2006, Australia
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Daniel R. Terno
Daniel R. Terno
a)
1
Department of Physics and Astronomy, Macquarie University
, Sydney, NSW 2109, Australia
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a)
Electronic mail: daniel.terno@mq.edu.au
Note: This paper is part of the special topic Celebrating Sir Roger Penrose's Nobel Prize.
AVS Quantum Sci. 4, 015606 (2022)
Article history
Received:
October 01 2021
Accepted:
February 04 2022
Citation
Pravin K. Dahal, Sebastian Murk, Daniel R. Terno; Semiclassical black holes and horizon singularities. AVS Quantum Sci. 1 March 2022; 4 (1): 015606. https://doi.org/10.1116/5.0073598
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