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.

arXiv comment7 pages, 8 figures, discussion concerning tidal forces added, interpretation of curvature brick wall corrected

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• Numerical evolution of the interior geometry of charged black holes
• Excision and avoiding the use of boundary conditions in numerical relativity
• On Nash theory of gravity with matter contents