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3D simulations of linearized scalar fields in Kerr spacetime

Mark A. Scheel·Adrienne L. Erickcek·Lior M. Burko·Lawrence E. Kidder·Harald P. Pfeiffer·Saul A. Teukolsky
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Abstract

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_lm(theta,phi) where Y_lm is a spherical harmonic and (r,theta,phi) are Kerr-Schild coordinates, to that of initial data proportional to f(r_BL) Y_lm(theta_BL,phi), where (r_BL,theta_BL) 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.

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Mark A. Scheel, Adrienne L. Erickcek, Lior M. Burko, Lawrence E. Kidder, Harald P. Pfeiffer, Saul A. Teukolsky. 2004-01-30. 3D simulations of linearized scalar fields in Kerr spacetime. https://doi.org/10.1103/physrevd.69.104006

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