A mystery of black-hole gravitational resonances

Abstract

More than three decades ago, Detweiler provided an analytical formula for the gravitational resonant frequencies of rapidly-rotating Kerr black holes. In the present work we shall discuss an important discrepancy between the famous {\it analytical} prediction of Detweiler and the recent {\it numerical} results of Zimmerman et. al. In addition, we shall refute the claim that recently appeared in the physics literature that the Detweiler-Teukolsky-Press resonance equation for the characteristic gravitational eigenfrequencies of rapidly-rotating Kerr black holes is not valid in the regime of damped quasinormal resonances with $\Im \omega /T_{\text{BH}}\gg 1$ (here $\omega$ and $T_{\text{BH}}$ are respectively the characteristic quasinormal resonant frequency of the Kerr black hole and its Bekenstein-Hawking temperature). The main goal of the present paper is to highlight and expose this important {\it black-hole quasinormal mystery} (that is, the intriguing discrepancy between the analytical and numerical results regarding the gravitational quasinormal resonance spectra of rapidly-rotating Kerr black holes).

9 pages. This is a slightly extended version of the one published in JCAP

References in corpus (7)

• Quasinormal modes of nearly extremal Kerr spacetimes: spectrum bifurcation and power-law ringdown
• Slow relaxation of rapidly rotating black holes
• Universal Bound on Dynamical Relaxation Times and Black-Hole Quasinormal Ringing
• Branching of quasinormal modes for nearly extremal Kerr black holes
• Quasinormal resonances of near-extremal Kerr-Newman black holes
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Cited by in corpus (3)

• Numerical computation of second order vacuum perturbations of Kerr black holes
• Spectroscopy of Extremal (and Near-Extremal) Kerr Black Holes
• Evolution of Fermion Resonance in Thick Brane