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
Gleiser, R., Nicasio, C., Price, R., & Pullin, J. (1998). Evolving the Bowen-York initial data for spinning black holes. Physical Review D - Particles, Fields, Gravitation and Cosmology, 57 (6), 3401-3407. https://doi.org/10.1103/PhysRevD.57.3401