Structure of the singularity inside a realistic rotating black hole

We present the structure and results of an analysis of the asymptotic behavior of nonlinear, asymmetric, metric perturbations near the Cauchy horizon inside a Kerr black hole. This analysis suggests that metric perturbations, to all orders in the perturbation expansion, are finite and small at the Cauchy horizon, even though their gradients (and the curvature) diverge there. Accordingly, objects which fall into a realistic rotating black hole a long time after the collapse will not be crushed by a tidal gravitational deformation as they approach the curvature singularity.

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