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

TL;DR

This paper derives an equally spaced entropy spectrum for d-dimensional spherically symmetric black holes using quasi-normal modes, connecting semi-classical analysis with quantum gravity insights.

Contribution

It extends the derivation of black hole entropy spectra to d dimensions using quasi-normal modes and relates it to microscopic quantum gravity models.

Findings

Entropy spectrum is equally spaced: S_{BH}=k ln(m_0)n

Large damping quasinormal mode frequency scales as  c/R_H(M)

Connection established between semi-classical analysis and quantum gravity models

Abstract

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.