2009/01/31 by Shao-Wen Wei, Ran Li, Yu-Xiao Liu +1 · 43 citations
Mathematics · Physics and Astronomy · #Adiabatic invariant #Adiabatic process #Black Holes and Theoretical Physics #Classical mechanics #Cosmology and Gravitation Theories #Entropy (arrow of time) #Equidistant #Geometry #Mathematical physics #Mathematics #Noncommutative and Quantum Gravity Theories #Physics #Quantization (signal processing) #Quantum mechanics #hep-th
paper · pdf · doi:10.1088/1126-6708/2009/03/076
published in Journal of High Energy Physics 2009(03), 076 (Springer Nature) · V3: 10 pages, the revised version emphasizes that the same result has been obtained earlier in Phys.Rev.D78(2008)104018[arXiv:0807.1481]
openalex publication_date 2009/03/11 · arxiv created 2009/03/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In Phys. Rev. D 78 (2008) 104018 [arXiv:0807.1481], the conclusion that "entropy eigenvalues of GB black hole are discrete and equally spaced, but the area spacing is not equidistant" was firstly presented by Kothawala, Padmanabhan and Sarkar. In this paper, using the new physical interpretation of quasinormal modes proposed by Maggiore, we calculate the quantum spectra of entropy for various types of non-rotating black holes with no charge. The spectrum is obtained by imposing Bohr-Sommerfeld quantization condition to the adiabatic invariant quantity. We conjecture that the spacing of entropy spectrum is equidistant and is independent of the dimension of spacetime. However, the spacing of area spectrum depends on gravity theory. In Einstein's gravity, it is equally spaced, otherwise it is non-equidistant. This conjecture agrees with the result of Kothawala, Padmanabhan and Sarkar.