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Evolving the Bowen-York initial data for spinning black holes

Reinaldo Gleiser·Oscar Nicasio·Richard Price·Jorge Pullin
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Abstract

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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Reinaldo Gleiser, Oscar Nicasio, Richard Price, Jorge Pullin. 1997-10-21. Evolving the Bowen-York initial data for spinning black holes. https://doi.org/10.1103/physrevd.57.3401

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