Outside a black hole, perturbation fields die off in time as 1/t n. For spherical holes n = 2ℓ + 3 where ℓ 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 ℓ 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 predictions. © 2008 IOP Publishing Ltd.
Publication Source (Journal or Book title)
Classical and Quantum Gravity
Gleiser, R., Price, R., & Pullin, J. (2008). Late-time tails in the Kerr spacetime. Classical and Quantum Gravity, 25 (7) https://doi.org/10.1088/0264-9381/25/7/072001