The Marolf-Ori singularity inside fast spinning black holes

Abstract

The effective shock wave singularity at the outgoing leg of the inner horizon of a linearly perturbed fast spinning black hole is studied numerically for either scalar field, or vacuum, gravitational perturbations. We demonstrate the occurrence of the Marolf-Ori singularity, including changes of order unity in the scalar field $\varphi$ for the scalar field model, and in the Weyl scalars ${\psi }_0$ and ${\psi }_4$ (rescaled appropriately by the horizon function $\Delta$) and the Kretschmann curvature scalar $K$ for the vacuum, gravitational perturbations model for both null and timelike geodesic observers. We quantify the shock sharpening effect and show that in all cases its rate agrees with expectations.

References in corpus (9)

• Structure of the black hole's Cauchy horizon singularity
• The physics of the relativistic counter-streaming instability that drives mass inflation inside black holes
• Outgoing gravitational shock-wave at the inner horizon: The late-time limit of black hole interiors
• Mode coupling mechanism for late-time Kerr tails
• Cauchy-horizon singularity inside perturbed Kerr black holes
• Numerical study of the gravitational shock wave inside a spherical charged black hole
• Inflation followed by Belinskii-Khalatnikov-Lifshitz collapse inside accreting, rotating black holes
• QED blue-sheet effects inside black holes
• Gravitational shock wave inside a steadily-accreting spherical charged black hole

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