The Radiative Tail of Realistic Gravitational Collapse
Abstract
An astrophysically realistic model of wave dynamics in black-hole spacetimes must involve a {\it non}-spherical background geometry with {\it angular momentum}. We consider the evolution of {\it gravitational} (and electromagnetic) perturbations in {\it rotating} Kerr spacetimes. We show that a rotating Kerr black hole becomes ``bald'' {\it slower} than the corresponding spherically-symmetric Schwarzschild black hole. Moreover, our results {\it turn over} the traditional belief (which has been widely accepted during the last three decades) that the late-time tail of gravitational collapse is universal. In particular, we show that different fields have {\it different} decaying rates. Our results are also of importance both to the study of the no-hair conjecture and the mass-inflation scenario (stability of Cauchy horizons).Keywords
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