Numerical evolution of shocks in the interior of Kerr black holes

Understand

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.