2008

Slow relaxation of rapidly rotating black holes

Hod, Shahar

Understand

We study analytically the relaxation phase of perturbed, rapidly rotating black holes.

In particular, we derive a simple formula for the fundamental quasinormal resonances of near-extremal Kerr black holes.
The formula is expressed in terms of the black-hole physical parameters: omega=m Omega-i2 pi T(n+1/2), where T and Omega are the temperature and angular velocity of the black hole, and m is the azimuthal harmonic index of a co-rotating equatorial mode.
This formula implies that the relaxation period tau sim 1/Im(omega) of the black hole becomes extremely long as the extremal limit T to 0 is approached.

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