Quasinormal ringing of Kerr black holes: The excitation factors

Details Quasinormal ringing of Kerr black holes: The excitation factors Quasinormal ringing of Kerr black holes: The excitation factors

2006-05-21

arxiv.org/abs/gr-qc/0605118v2

Phys.Rev. D74 (2006) 104020

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

33 pages, 9 figures, 7 tables, RevTeX4. v2: Two new figures and minor changes in the presentation. Matches version in press in

Scientific paper

10.1103/PhysRevD.74.104020

Distorted black holes radiate gravitational waves. In the so-called ringdown phase radiation is emitted in a discrete set of complex quasinormal frequencies, whose values depend only on the black hole's mass and angular momentum. Ringdown radiation could be detectable with large signal-to-noise ratio by the Laser Interferometer Space Antenna LISA. If more than one mode is detected, tests of the black hole nature of the source become possible. The detectability of different modes depends on their relative excitation, which in turn depends on the cause of the perturbation (i.e. on the initial data). A ``universal'', initial data-independent measure of the relative mode excitation is encoded in the poles of the Green's function that propagates small perturbations of the geometry (``excitation factors''). We compute for the first time the excitation factors for general-spin perturbations of Kerr black holes. We find that for corotating modes with $l=m$ the excitation factors tend to zero in the extremal limit, and that the contribution of the overtones should be more significant when the black hole is fast rotating. We also present the first analytical calculation of the large-damping asymptotics of the excitation factors for static black holes, including the Schwarzschild and Reissner-Nordstrom metrics. This is an important step to determine the convergence properties of the quasinormal mode expansion.

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