Numerical Evolution in time of curvature perturbations in Kerr black holes

Details Numerical Evolution in time of curvature perturbations in Kerr black holes Numerical Evolution in time of curvature perturbations in Kerr black holes

1999-11-02

arxiv.org/abs/gr-qc/9911006v1

AMS/IP Stud.Adv.Math.13:377-385,1999

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

RevTex, 6 pages. Appeared in proceedings of "Trends in Mathematical Physics" Conference; UT, Knoxville Oct. 14-17,1998

Scientific paper

This paper reviews the basic features of the theory of curvature perturbations in Kerr spacetime, which is customarily written in terms of gauge invariant components of the Weyl tensor which satisfy a perturbation equation known as the Teukolsky equation. I will describe how to evolve generic perturbations about the Kerr metric and the separable form of the wave solutions that one obtains, and the relation of the Teukolsky function to the energy of gravitational waves emitted by the black hole. A discussion of a numerical scheme to evolve perturbations as a function of time and some preliminary results of our research project implementing it for matter sources falling into the black hole is included.

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