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Thermodynamical Properties of Horizons

J. Makela·A. Peltola
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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.

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J. Makela, A. Peltola. 2002-05-30. Thermodynamical Properties of Horizons. https://arxiv.org/abs/gr-qc/0205128

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