Rotating Black Hole Interiors, Proper Time Structure, and Implications for Cosmological Bounce

Black holes represent one of the most extreme predictions of general relativity, where spacetime curvature becomes strong enough to form event horizons and classical singularities. While the Schwarzschild solution provides a simple model of a non-rotating black hole, astrophysical black holes are expected to possess angular momentum and are therefore better described by the Kerr geometry. One of the long-standing problems in black hole physics concerns the nature of singularities and the fate of information. Classical general relativity predicts geodesic incompleteness, while semiclassical arguments introduce Hawking radiation and the associated information paradox. More recent developments, such as the Page curve and holographic dualities, suggest that information is preserved, though its precise dynamical mechanism remains unclear. In this work, we investigate the proper-time structure of rotating black hole interiors and examine whether their causal structure allows for short-lived internal evolution compatible with nonsingular, high-curvature transition scenarios. Such scenarios may provide a geometric basis for bounce-like behavior and potential parameter inheritance mechanisms relevant for cosmological models.