  Here we present a novel classical model to describe the near-inner horizon
geometry of a rotating, accreting black hole. The model assumes spacetime is
homogeneous and is sourced by radial streams of a collisionless, null fluid,
and it predicts that the standard Poisson-Israel mass inflation phenomenon will
be interrupted by a Kasner-like collapse toward a spacelike singularity. Such a
model is shown to be valid at the inner horizon of astrophysically realistic
black holes through comparison to the conformally-separable model, which
provides a natural connection of the Kerr metric to a self-similar, accreting
spacetime. We then analyze the behavior of null geodesics in our model,
connecting them to the Kerr metric in order to answer the practical question of
what an infalling observer approaching the inner horizon might see.
