The Entropy Function for the Black Holes of Nariai Class

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dc.creatorCho, Jin-Ho
dc.creatorNam, Soonkeon
dc.date2007-11-15
dc.date2008-03-10
dc.date.accessioned2026-07-07T11:13:13Z
dc.date.available2026-07-07T11:13:13Z
dc.descriptionBased on the fact that the near horizon geometry of the extremal Schwarzschild-de Sitter black holes is Nariai geometry, we define the black holes of Nariai class as the configuration whose near-horizon geometry is factorized as two dimensional de Sitter space-time and some compact topology, that is Nariai geometry. We extend the entropy function formalism to the case of the black holes of Nariai class. The conventional entropy function (for the extremal black holes) is defined as Legendre transformation of Lagrangian density, thus the `Routhian density', over two dimensional anti-de Sitter. As for the black holes of Nariai class, it is defined as {\em minus} `Routhian density' over two dimensional de Sitter space-time. We found an exact agreement of the result with Bekenstein-Hawking entropy. The higher order corrections are nontrivial only when the space-time dimension is over four, that is, $d>4$. There is a subtlety as regards the temperature of the black holes of Nariai class. We show that in order to be consistent with the near horizon geometry, the temperature should be non-vanishing despite the extremality of the black holes.
dc.descriptionreferences added, compatible with the published version
dc.identifierhttps://arxiv.org/abs/0711.2514
dc.identifierhttp://arxiv.org/abs/0711.2514
dc.identifierJHEP0803:027,2008
dc.identifierdoi:10.1088/1126-6708/2008/03/027
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/191644
dc.subjectHigh Energy Physics - Theory
dc.titleThe Entropy Function for the Black Holes of Nariai Class
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