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Highly Damped Quasinormal Modes of Kerr Black Holes: A Complete Numerical Investigation

Emanuele Berti·Vitor Cardoso·Shijun Yoshida
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Abstract

We compute for the first time very highly damped quasinormal modes of the (rotating) Kerr black hole. Our numerical technique is based on a decoupling of the radial and angular equations, performed using a large-frequency expansion for the angular separation constant_{s}A_{l m}. This allows us to go much further in overtone number than ever before. We find that the real part of the quasinormal frequencies approaches a non-zero constant value which does not depend on the spin s of the perturbing field and on the angular index l: ω_R=m\varpi(a). We numerically compute \varpi(a). Leading-order corrections to the asymptotic frequency are likely to be of order 1/ω_I. The imaginary part grows without bound, the spacing between consecutive modes being a monotonic function of a.

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Emanuele Berti, Vitor Cardoso, Shijun Yoshida. 2004-01-13. Highly Damped Quasinormal Modes of Kerr Black Holes: A Complete Numerical Investigation. https://doi.org/10.1103/physrevd.69.124018

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