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arXiv · 0710.4183

Late time tails in the Kerr spacetime

Reinaldo J. Gleiser·Richard H. Price·Jorge Pullin
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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.

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Reinaldo J. Gleiser, Richard H. Price, Jorge Pullin. 2013-05-27. Late time tails in the Kerr spacetime. https://doi.org/10.1088/0264-9381%2F25%2F7%2F072001

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