Evolving the Bowen-York initial data for boosted black holes

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Abstract
The Bowen-York initial value data typically used in numerical relativity to represent boosted black holes are not those of a constant-time slice of the a boosted Schwarzschild 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 ``boosted Schwarzschild'' form. We compute this radiation by treating the geometry for a single boosted Bowen-York hole as a perturbation of a boosted Schwarzschild black hole, and by using second order perturbation theory. We discuss the extent to which Bowen-York data can be expected to represent accurately boosted Schwarzschild holes for the purpose of black hole collisions.

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