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 [Formula Presented] 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 nonzero constant value which does not depend on the spin s of the perturbing field or on the angular index l: [Formula Presented] We numerically compute [Formula Presented] Leading-order corrections to the asymptotic frequency are likely to be [Formula Presented] The imaginary part grows without bound, the spacing between consecutive modes being a monotonic function of a.
|Journal||Physical Review D - Particles, Fields, Gravitation and Cosmology|
|Publication status||Published - 2004 Jan 1|
ASJC Scopus subject areas
- Nuclear and High Energy Physics
- Physics and Astronomy (miscellaneous)