Thermodynamical Properties of Horizons

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dc.creatorMakela, J.
dc.creatorPeltola, A.
dc.date2002-05-30
dc.date.accessioned2026-07-07T03:26:54Z
dc.date.available2026-07-07T03:26:54Z
dc.descriptionWe 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.
dc.description13 pages, 3 figures
dc.identifierhttps://arxiv.org/abs/gr-qc/0205128
dc.identifierhttp://arxiv.org/abs/gr-qc/0205128
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/34232
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleThermodynamical Properties of Horizons
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