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/

Zendy Open

Presents the pdf analysis as premium feature

PDF Analysis

Insights

Presents the summarisation as premium feature

Summarisation

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the zaia usage as premium feature

ZAIA

Zendy Tools

Zendy Plus

Presents the access of premium content as premium feature

Premium Content

We estimate the canonical entropy of a quantum black hole by counting itsquasi-normal modes. We first show that the partition function of a classicalblack hole, evaluated by counting the quasi-normal modes with a thermodyanmicBoltzmann weight, leads to a small entropy of order unity due to the smallcontribution from higher angular modes. We then discuss how this will bemodified when taking into account dissipation effects near the horizon due tointeraction with the quantum black hole microstates. The structure ofquasi-normal modes drastically changes, yielding a fundamental frequency of theinverse of $t_{\rm echo} \sim$ log(Entropy)/Temperature. This is the time-scalefor reflection from the microstates (or the quantum time limit of silence,followed by echoes), $\textit{independent of the strength of dissipation}$, andis comparable to the scrambling time proposed by Sekino & Susskind. Setting thedissipation constant to Planck time, we reproduce the Bekenstein-Hawkingentropy of $\sim$ (Horizon area)/(Planck area). This result suggests thepossibility of simulating black hole entropy in analog horizons realized incondensed matter systems.

From Entropy to Echoes: Counting the quasi-normal modes and the quantum limit of silence