Scheel, Mark A. and Erickcek, Adrienne L. and Burko, Lior M. and Kidder, Lawrence E. and Pfeiffer, Harald P. and Teukolsky, Saul A. (2004) 3D simulations of linearized scalar fields in Kerr spacetime. Physical Review D, 69 (10). Art. No. 104006. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:SCHEprd04
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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)Y[script l]m(theta,phi), where Y[script l]m is a spherical harmonic and (r,theta,phi) are Kerr-Schild coordinates, to that of initial data proportional to f(rBL)Y[script l]m(thetaBL,phi), where (rBL,thetaBL) 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.
|Additional Information:||©2004 The American Physical Society (Received 6 May 2003; published 12 May 2004) We thank Lee Lindblom and Richard Price for valuable discussions. Some computations were performed on the IA-32 Linux cluster at NCSA. This research was supported in part by NSF grant PHY-0099568 at the California Institute of Technology, NSF grant PHY-9900672 at Cornell University, and NSF grants PHY-9734871 and PHY-0244605 at the University of Utah. A.L.E. was supported by the LIGO Summer Undergraduate Research Program at the California Institute of Technology. L.M.B. thanks Kip Thorne for hospitality at Caltech during the beginning phase of this work.|
|Subject Keywords:||space-time configurations; black holes; perturbation theory|
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|Deposited By:||Archive Administrator|
|Deposited On:||24 Feb 2006|
|Last Modified:||26 Dec 2012 08:46|
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