Dynamics of spin-2 fields in Kerr background geometries

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We have developed a numerical method for evolving perturbations of rotating black holes. Solutions are obtained by integrating the Teukolsky equation written as a first-order in time, coupled system of equations, in a form that explicitly exhibits the radial characteristic directions. We follow the propagation of generic initial data through the burst, quasi-normal ringing and power-law tail phases. Future results may help to clarify the role of black hole angular momentum on signals produced during the final stages of black hole coalescence.
3 pages LaTeX using sprocl.sty, 1 figure, to appear in: Proceedings of the 18th Texas Symposium on Relativistic Astrophysics (eds Olinto, Frieman and Schramm, World Scientific)

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General Relativity and Quantum Cosmology

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http://salesiana.dossiersoluciones.com/handle/123456789/35862

Consulte el texto completo en el siguiente enlace:

https://arxiv.org/abs/gr-qc/9701036
 http://arxiv.org/abs/gr-qc/9701036

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arXiv