Numerical evolution of shocks in the interior of Kerr black holes
General Relativity and Quantum Cosmology
2019-04-24 v3
Abstract
We numerically solve Einstein's equations coupled to a scalar field in the interior of Kerr black holes. We find shock waves form near the inner horizon. The shocks grow exponentially in amplitude and need not be axisymmetric. Observers who pass through the shocks experience exponentially large tidal forces and are accelerated exponentially close to the speed of light.
Cite
@article{arxiv.1808.07502,
title = {Numerical evolution of shocks in the interior of Kerr black holes},
author = {Paul M. Chesler and Erik Curiel and Ramesh Narayan},
journal= {arXiv preprint arXiv:1808.07502},
year = {2019}
}
Comments
7 pages, 8 figures, discussion concerning tidal forces added, interpretation of curvature brick wall corrected