Thermodynamical Properties of Horizons
General Relativity and Quantum Cosmology
2007-05-23 v1
Abstract
We show, by using Regge calculus, that the entropy of any finite part of a Rindler horizon is, in the semi-classical limit, one quarter of the area of that part. We argue that this result implies that the entropy associated with any horizon of spacetime is, in semi-classical limit, one quarter of its area. As an example, we derive the Bekenstein-Hawking entropy law for the Schwarzschild black hole.
Cite
@article{arxiv.gr-qc/0205128,
title = {Thermodynamical Properties of Horizons},
author = {J. Makela and A. Peltola},
journal= {arXiv preprint arXiv:gr-qc/0205128},
year = {2007}
}
Comments
13 pages, 3 figures