Quasi-spherical approximation for rotating black holes

Details Quasi-spherical approximation for rotating black holes Quasi-spherical approximation for rotating black holes

2000-08-30

arxiv.org/abs/gr-qc/0008075v2

Phys.Rev. D64 (2001) 044002

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

revised version, 8 pages, RevTeX, 8 figures, epsf.sty, psfrag.sty, graphicx.sty

Scientific paper

10.1103/PhysRevD.64.044002

We numerically implement a quasi-spherical approximation scheme for computing gravitational waveforms for coalescing black holes, testing it against angular momentum by applying it to Kerr black holes. As error measures, we take the conformal strain and specific energy due to spurious gravitational radiation. The strain is found to be monotonic rather than wavelike. The specific energy is found to be at least an order of magnitude smaller than the 1% level expected from typical black-hole collisions, for angular momentum up to at least 70% of the maximum, for an initial surface as close as $r=3m$.

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