3D simulations of linearized scalar fields in Kerr spacetime

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Abstract
We investigate the behavior of a dynamical scalar field on a fixed Kerr background 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 a spherical harmonic Y_lm(theta,phi), where (theta,phi) are Kerr-Schild coordinates, to that of initial data proportional to Y_lm(theta_BL,phi), where theta_BL is the Boyer-Lindquist coordinate. 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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