Thermodynamics of Black Holes from Equipartition of Energy and Holography
arXiv:1002.1275 · doi:10.1103/PhysRevD.81.104013
Abstract
A gravitational potential in the relativistic case is introduced as an alternative to Wald's potential used by Verlinde, which reproduces the familiar entropy/area relation S=A/4 (in the natural units) when Verlinde's idea is applied to the black hole case. Upon using the equipartition rule, the correct form of the Komar mass (energy) can also be obtained, which leads to the Einstein equations. It is explicitly shown that our entropy formula agrees with Verlinde's entropy variation formula in spherical cases. The stationary space-times, especially the Kerr-Newman black hole, are then discussed, where it is shown that the equipartition rule involves the reduced mass, instead of the ADM mass, on the horizon of the black hole.
arXiv comment13 pages, a discussion is added into section III in the new version, which explicitly shows that our entropy formula agrees with Verlinde's entropy variation formula in spherical cases. The abstract, introduction and conluding remarks also have been revised. Some typing mistakes in old versions have been corrected. v4: minor modifications, match the published version.
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