Shahar Hod

Bohr's correspondence principle and the area spectrum of quantum black holes

During the last twenty-five years evidence has been mounting that a black-hole surface area has a discrete spectrum. Moreover, it is widely believed that area eigenvalues are uniformly spaced. There is, however, no general agreement on the spacing of the levels. In this Letter we use Bohrs correspondence principle to provide this missing link. We conclude that the area spacing of a black hole is

Slow relaxation of rapidly rotating black holes

4\ensuremath{\Elzxh}\mathrm{ln}3

Universal bound on dynamical relaxation times and black-hole quasinormal ringing

. This is the unique spacing consistent both with the area-entropy thermodynamic relation for black holes, with the Boltzmann-Einstein formula in statistical physics, and with Bohrs correspondence principle.

Stationary resonances of rapidly-rotating Kerr black holes

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:

Kerr-Newman black holes with stationary charged scalar clouds

\ensuremath{\omega}=m\ensuremath{\Omega}\ensuremath{-}i2\ensuremath{\pi}{T}_{\mathrm{BH}}(n+\frac{1}{2})

Best Approximation to a Reversible Process in Black-Hole Physics and the Area Spectrum of Spherical Black Holes

, where

Weak cosmic censorship: as strong as ever.

{T}_{\mathrm{BH}}

On the instability regime of the rotating Kerr spacetime to massive scalar perturbations

and

Analytic Study of Rotating Black-Hole Quasinormal Modes

\ensuremath{\Omega}

Stability of the extremal Reissner–Nordström black hole to charged scalar perturbations

are the temperature and angular velocity of the black hole, and