Thermodynamical Properties of Horizons

TL;DR

This paper demonstrates that the entropy of any finite horizon segment in spacetime, including black holes, is proportional to its area, supporting the universal nature of horizon entropy in semi-classical gravity.

Contribution

It provides a semi-classical derivation of horizon entropy using Regge calculus, extending the Bekenstein-Hawking law to general horizons.

Findings

Horizon entropy equals one quarter of the area in semi-classical limit

Derivation of Bekenstein-Hawking entropy for Schwarzschild black hole

Universal applicability of area-entropy relation for spacetime horizons

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.