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 $n=2ell+3$ 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.