Numerical evolution of shocks in the interior of Kerr black holes

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.

7 pages, 8 figures, discussion concerning tidal forces added, interpretation of curvature brick wall corrected