Quasinormal modes and horizon area quantisation in Loop Quantum Gravity

Abstract

It is argued that the quantum of area between consecutive, high overtones quasinormal modes of a black hole horizon coincides with the area gap predicted by Loop Quantum Gravity, as long as the horizon is isolated and the Barbero-Immirzi parameter is $\gamma \approx \sqrt{3}/6$, in agreement with the value derived from the Bekenstein-Hawking horizon entropy.

9 pages, two figures, version to appear in General Relativity and Gravitation

References in corpus (4)

• The physical interpretation of the spectrum of black hole quasinormal modes
• Potential gravitational-wave signatures of quantum gravity
• Flux-area operator and black hole entropy
• Spectral Lines of Quantized, Spinning Black Holes and their Astrophysical Relevance

Cited by in corpus (4)

• Primordial black holes in loop quantum cosmology: The effect on the threshold
• Breaking of isospectrality of quasinormal modes in nonrotating loop quantum gravity black holes
• On the horizon area of effective loop quantum black holes
• Constraining the Barbero-Immirzi parameter from the duration of inflation in loop quantum cosmology