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Titolo:
Statistical entropies of scalar and spinor fields in Vaidya-de Sitter space-time computed by the thin-layer method - art. no. 044025
Autore:
He, F; Zhao, Z; Kim, SW;
Indirizzi:
Beijing Normal Univ, Dept Phys, Beijing 100875, Peoples R China Beijing Normal Univ Beijing Peoples R China 100875 0875, Peoples R China Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea Ewha Womans Univ Seoul South Korea 120750 duc, Seoul 120750, South Korea Xiang Tan Normal Univ, Dept Phys, Xiangtan 411201, Peoples R China Xiang Tan Normal Univ Xiangtan Peoples R China 411201 1, Peoples R China
Titolo Testata:
PHYSICAL REVIEW D
fascicolo: 4, volume: 6404, anno: 2001,
pagine: 4025 -
SICI:
0556-2821(20010815)6404:4<4025:SEOSAS>2.0.ZU;2-G
Fonte:
ISI
Lingua:
ENG
Soggetto:
NEWMAN BLACK-HOLE; THERMODYNAMICS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
--discip_EC--
Citazioni:
17
Recensione:
Indirizzi per estratti:
Indirizzo: He, F Beijing Normal Univ, Dept Phys, Beijing 100875, Peoples R China Beijing Normal Univ Beijing Peoples R China 100875 Peoples R China
Citazione:
F. He et al., "Statistical entropies of scalar and spinor fields in Vaidya-de Sitter space-time computed by the thin-layer method - art. no. 044025", PHYS REV D, 6404(4), 2001, pp. 4025

Abstract

The brick-wall method based on thermal equilibrium at a large scale cannotbe applied to cases out of equilibrium, such as nonstationary space-time with two horizons, for example, Vaidya-de Sitter space-time. We improve the brick-wall method and propose a thin-layer method. The entropies of scalar and spinor fields in Vaidya-de Sitter space-time are calculated by the thin-layer method, The condition of local equilibrium near the two horizons is used as a working postulate and is maintained for a black hole which evaporates slowly enough and whose mass is far greater than the Planck scale. There are two horizons in Vaidya-de Sitter space-time. We think that the totalentropy is mainly attributed to the two layers near the two horizons. The entropy of a scalar field in Vaidya-de Sitter space-time is a linear sum ofthe area of the black hole horizon and that of the cosmological horizon. Thinking of Dirac equations in the Newman-Penrose formalism, there are four components of the wave functions F-1, F-2, G(1), and G(2). The total entropy is summed up from the entropies corresponding to the four components. On the same condition of the scalar field, the resulting entropy is 7/2 times that of the scalar field, and is also a linear sum of the area of the blackhole horizon and that of the cosmological horizon. The difference from thestationary black hole is that the result relies on time-dependent cutoffs.

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Documento generato il 23/09/20 alle ore 00:17:42