1997/10/21 by Reinaldo J. Gleiser, Reinaldo Gleiser, Carlos O. Nicasio +4
Engineering · Physics and Astronomy · #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Classical mechanics #Computer science #General relativity #Geophysics and Sensor Technology #Gravitational collapse #Gravitational wave #Hawking radiation #Kerr metric #Numerical relativity #Perturbation (astronomy) #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Rotating black hole #Schwarzschild metric #Schwarzschild radius #Spacetime #Spinning #Theory of relativity #White hole #gr-qc
paper · pdf · doi:10.1103/physrevd.57.3401
published as Phys.Rev. D57 (1998) 3401-3407 · 10 pages, RevTeX, 4 figures included with psfig
arxiv created 1997/10/21 · openalex publication_date 1998/03/15 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
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.