Radiative Tail of Realistic Rotating Gravitational Collapse

An astrophysically realistic model of wave dynamics in black-hole spacetimes must involve a non-spherical background geometry with angular momentum. We consider the evolution of gravitational (and electromagnetic) perturbations in rotating Kerr spacetimes. We show that a rotating Kerr black hole bec...

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Bibliographic Details
Published inarXiv.org
Main Author Hod, Shahar
Format Paper
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 02.01.2000
Subjects
Angular momentum
Gravitation
Gravitational collapse
Rotation
Spacetime
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Summary:An astrophysically realistic model of wave dynamics in black-hole spacetimes must involve a non-spherical background geometry with angular momentum. We consider the evolution of gravitational (and electromagnetic) perturbations in rotating Kerr spacetimes. We show that a rotating Kerr black hole becomes `bald' slower than the corresponding spherically-symmetric Schwarzschild black hole. Moreover, our results 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 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).
ISSN:2331-8422
DOI:10.48550/arxiv.9907096