d-Dimensional Black Hole Entropy Spectrum from Quasi-Normal Modes

Details d-Dimensional Black Hole Entropy Spectrum from Quasi-Normal Modes d-Dimensional Black Hole Entropy Spectrum from Quasi-Normal Modes

2002-12-03

arxiv.org/abs/gr-qc/0212014v2

Phys.Rev.Lett.90:161301,2003

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

4 pages, Latex, Revtex4 Some formulas corrected, a reference added

Scientific paper

10.1103/PhysRevLett.90.161301

Starting from recent observations\cite{hod,dreyer1} about quasi-normal modes, we use semi-classical arguments to derive the Bekenstein-Hawking entropy spectrum for $d$-dimensional spherically symmetric black holes. We find that the entropy spectrum is equally spaced: $S_{BH}=k \ln(m_0)n$, where $m_0$ is a fixed integer that must be derived from the microscopic theory. As shown in \cite{dreyer1},4-$d$ loop quantum gravity yields precisely such a spectrum with $m_0=3$ providing the Immirzi parameter is chosen appropriately. For $d$-dimensional black holes of radius $R_H(M)$, our analysis requires the existence of a unique quasinormal mode frequency in the large damping limit $\omega^{(d)}(M) = \alpha^{(d)}c/ R_H(M)$ with coefficient $\alpha^{(d)} = {(d-3)/over 4\pi} \ln(m_0)$, where $m_0$ is an integer and $\Gamma^{(d-2)}$ is the volume of the unit $d-2$ sphere.

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