2003/03/31 by Emanuele Berti, Kostas D. Kokkotas · 4 citations
Physics and Astronomy · #Angular momentum #Black Holes and Theoretical Physics #Black hole (networking) #Charge (physics) #Classical mechanics #General relativity #Gravitation #Mathematical physics #Noncommutative and Quantum Gravity Theories #Omega #Physics #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Quantum mechanics #Quasinormal mode #Rotating black hole #Schwarzschild radius #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.68.044027
published as Phys.Rev. D68 (2003) 044027 · 13 pages, 7 figures. Added result on the asymptotic spacing of the imaginary part, minor typos corrected
arxiv created 2003/06/23 · openalex publication_date 2003/08/28 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
According to a recent proposal, the so-called Barbero-Immirzi parameter of loop quantum gravity can be fixed, using Bohr's correspondence principle, from a knowledge of highly damped black hole oscillation frequencies. Such frequencies are rather difficult to compute, even for Schwarzschild black holes. However, it is now quite likely that they may provide a fundamental link between classical general relativity and quantum theories of gravity. Here we carry out the first numerical computation of very highly damped quasinormal modes (QNM's) for charged and rotating black holes. In the Reissner-Nordstr"om case QNM frequencies and damping times show an oscillatory behavior as a function of charge. The oscillations become faster as the mode order increases. At fixed mode order, QNM's describe spirals in the complex plane as the charge is increased, tending towards a well defined limit as the hole becomes extremal. Kerr QNM's have a similar oscillatory behavior when the angular index m=0. For l=m=2 the real part of Kerr QNM frequencies tends to 2\ensuremathΩ, \ensuremathΩ being the angular velocity of the black hole horizon, while the asymptotic spacing of the imaginary parts is given by 2\ensuremathπTH.