A numerical method that excises the outer computational boundary along the ingoing light cone makes boundary conditions unnecessary, at the cost of limiting evolution to about one light-crossing time of the initial grid.
Numerical evolution of shocks in the interior of Kerr black holes
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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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gr-qc 1years
2019 1verdicts
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Excision and avoiding the use of boundary conditions in numerical relativity
A numerical method that excises the outer computational boundary along the ingoing light cone makes boundary conditions unnecessary, at the cost of limiting evolution to about one light-crossing time of the initial grid.