Document Type

Article

Publication Date

1-1-1998

Abstract

The Bowen-York initial value data typically used in numerical relativity to represent a 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. © 1998 The American Physical Society.

Publication Source (Journal or Book title)

Physical Review D - Particles, Fields, Gravitation and Cosmology

First Page

3401

Last Page

3407

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