Thermodynamics of de Sitter Black Holes: Thermal Cosmological Constant

By Y. Sekiwa. 2006

233 citations recorded by the source corpus.

We study the thermodynamic properties associated with the black hole event horizon and the cosmological horizon for black hole solutions in asymptotically de Sitter spacetimes. We examine thermodynamics of these horizons on the basis of the conserved charges according to Teitelboim's method. In particular, we have succeeded in deriving the generalized Smarr formula among thermodynamical quantities in a simple and natural way. We then show that cosmological constant must decrease when one takes into account the quantum effect. These observations have been obtained if and only if the cosmological constant plays the role of a thermodynamical state variable. We also touch upon the relation between inflation of our universe and a phase transition of black holes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/38f548f4bcb3abaa18593ead2df0b88a3178d9af

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Citations in the corpus

Enthalpy and the mechanics of AdS black holes (2009, methodology): “In fact, similar expressions for the (A)dS Smarr formula and the first law with variable Λ have been obtained before in references [17, 18, 19, 20, 21, 22].”
Holographic heat engines (2014, unknown): “[5–13], including the reviews in refs.”
The mechanical first law of black hole spacetimes with a cosmological constant and its application to the Schwarzschild–de Sitter spacetime (2009, unknown): “0264-9381/09/105010+14$30.00 © 2009 IOP Publishing Ltd Printed in the UK 1”
Thermodynamic Volumes and Isoperimetric Inequalities for de Sitter Black Holes (2013, result): “2 Similar results have been obtained by Cai [22, 23] and by Sekiwa [24] in more limited contexts (see also [25] and [26]).”
Black hole chemistry: thermodynamics with Lambda (2016, background): “positive root r b, and the inner horizon (if it exists) corresponds to the third largest positive r i (denoted with subscript i). The arguments in App. A can be recapitulated for >0 [49] (see also [244, 245, 246]), and indicate that the following rst laws: M= T bS b+ X k k b J k+ X j jQj+V bP; (6”
Thermodynamics of Rotating Black Holes and Black Rings: Phase Transitions and Thermodynamic Volume (2014, background): “Extensions of this idea to asymptotically de Sitter space times have also been recently explored, with the resultant thermodynamic notions for black holes remaining intact [40] (see also [41–49]).”