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arXiv · 1808.07502

Numerical evolution of shocks in the interior of Kerr black holes

Paul M. Chesler·Erik Curiel·Ramesh Narayan
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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.

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Paul M. Chesler, Erik Curiel, Ramesh Narayan. 2018-08-22. Numerical evolution of shocks in the interior of Kerr black holes. https://doi.org/10.1103/physrevd.99.084033

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