Late time tails in the Kerr spacetime

Abstract

Outside a black hole, perturbation fields die off in time as $1/t^n$. For spherical holes $n=2\ell +3$ where $\ell$ is the multipole index. In the nonspherical Kerr spacetime there is no coordinate-independent meaning of "multipole," and a common sense viewpoint is to set $\ell$ to the lowest radiatiable index, although theoretical studies have led to very different claims. Numerical results, to date, have been controversial. Here we show that expansion for small Kerr spin parameter $a$ leads to very definite numerical results confirming previous theoretical analyses.

4 pages, 1 figure. In previous version an important modification of the radial variable was omitted

References in corpus (4)

• 3D simulations of linearized scalar fields in Kerr spacetime
• High accuracy simulations of Kerr tails: coordinate dependence and higher multipoles
• Radiative falloff in the background of rotating black hole
• Radiative falloff of a scalar field in a weakly curved spacetime without symmetries

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