English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Starting from recent observations\cite{hod,dreyer1} about quasi-normal modes,we use semi-classical arguments to derive the Bekenstein-Hawking entropyspectrum for $d$-dimensional spherically symmetric black holes. We find thatthe entropy spectrum is equally spaced: $S_{BH}=k \ln(m_0)n$, where $m_0$ is afixed 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 theexistence 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 $\Gamma^{(d-2)}$ isthe volume of the unit $d-2$ sphere.Comment: 4 pages, Latex, Revtex4 Some formulas corrected, a reference adde

physical review letters

<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>d</mml:mi></mml:math>-Dimensional Black Hole Entropy Spectrum from Quasinormal Modes

d-Dimensional Black Hole Entropy Spectrum from Quasinormal Modes