2003/05/31 by Mark Scheel, Mark A. Scheel, Adrienne L. Erickcek +5 · 4 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Pulsars and Gravitational Waves Research #gr-qc
paper · pdf · doi:10.1103/physrevd.69.104006
published as Phys.Rev. D69 (2004) 104006 · 12 pages, 9 figures, revtex4. Major revision: added figures, added subsection on convergence, clarified discussion. To appear in Phys Rev D
arxiv created 2004/01/30 · openalex publication_date 2004/05/12 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We investigate the behavior of a dynamical scalar field on a fixed Kerr background in Kerr-Schild coordinates using a (3+1)-dimensional spectral evolution code, and we measure the power-law tail decay that occurs at late times. We compare evolutions of initial data proportional to f(r)Ylm(\ensuremathθ,\ensuremathφ), where Ylm is a spherical harmonic and (r,\ensuremathθ,\ensuremathφ) are Kerr-Schild coordinates, to that of initial data proportional to f(rBL)Ylm(\ensuremathθBL,\ensuremathφ), where (rBL,\ensuremathθBL) are Boyer-Lindquist coordinates. We find that although these two cases are initially almost identical, the evolution can be quite different at intermediate times; however, at late times the power-law decay rates are equal.