Evolving the Bowen-York initial data for spinning black holes

Details Evolving the Bowen-York initial data for spinning black holes Evolving the Bowen-York initial data for spinning black holes

1997-10-21

arxiv.org/abs/gr-qc/9710096v1

Phys.Rev. D57 (1998) 3401-3407

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

10 pages, RevTeX, 4 figures included with psfig

Scientific paper

10.1103/PhysRevD.57.3401

The Bowen-York initial value data typically used in numerical relativity to represent spinning black hole are not those of a constant-time slice of the Kerr spacetime. If Bowen-York initial data are used for each black hole in a collision, the emitted radiation will be partially due to the ``relaxation'' of the individual holes to Kerr form. We compute this radiation by treating the geometry for a single hole as a perturbation of a Schwarzschild black hole, and by using second order perturbation theory. We discuss the extent to which Bowen-York data can be expected accurately to represent Kerr holes.

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