Inside astronomically realistic black holes
Abstract
The singularity of a spherical (Schwarzschild) black hole is a surface, not a point. A freely-falling, non-rotating observer sees Hawking radiation with energy density diverging with radius as near the Schwarzschild singular surface. Spacetime inside a rotating (Kerr) black hole terminates at the inner horizon because of the Poisson-Israel mass inflation instability. If the black hole is accreting, as all realistic black holes do, then generically inflation gives way to Belinski-Khalatnikov-Lifshitz oscillatory collapse to a strong, spacelike singular surface.
Cite
@article{arxiv.1907.05292,
title = {Inside astronomically realistic black holes},
author = {Andrew J. S. Hamilton},
journal= {arXiv preprint arXiv:1907.05292},
year = {2019}
}
Comments
18 pages, invited plenary talk, to be published in the Proceedings of the Fifteenth Marcel Grossmann Meeting on General Relativity, July 2018, ed. Elia Battistelli, Robert T. Jantzen, and Remo Ruffini