Action and entropy of black holes in spacetimes with a cosmological constant

Cai, Rong-Gen; Ji, Jeong‐Young; Soh, Kwang–Sup

doi:10.1088/0264-9381/15/9/023

Cited by 88 publications

(71 citation statements)

References 24 publications

(48 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The situation we have is identical to that for the lukewarm RNdS black holes without a scalar field [5,6], namely the action (25) does not equal minus the total entropy. However, as discussed in [6,18], we are dealing with an instanton manifold of finite spatial extent and so our action I E is the microcanonical action, which means that the entropy S must be given by S = −I E [18].…”

Section: Entropy and Euclidean Actionmentioning

confidence: 62%

Thermodynamics of de Sitter black holes with a conformally coupled scalar field

2005

View full text Add to dashboard Cite

We study the thermodynamics of de Sitter black holes with a conformally coupled scalar field. The geometry is that of the "lukewarm" Reissner-Nordström-de Sitter black holes, with the event and cosmological horizons at the same temperature. This means that the region between the event and cosmological horizons can form a regular Euclidean instanton. The entropy is modified by the non-minimal coupling of the scalar field to the geometry, but can still be derived from the Euclidean action, provided suitable modifications are made to deal with the electrically charged case. We use the first law as derived from the isolated horizons formalism to compute the local horizon energies for the event and cosmological horizons.

show abstract

Section: Entropy and Euclidean Actionmentioning

confidence: 62%

Thermodynamics of de Sitter black holes with a conformally coupled scalar field

2005

View full text Add to dashboard Cite

show abstract

“…Especially researchers pay widespread attention to the statistical origin of the black hole entropy. Many methods of calculating entropy have emerged [4][5][6][7][8][9]. One of them is the well-known brick-wall method [7].…”

Section: Introductionmentioning

confidence: 99%

Entropy of Kerr-Newman Black Hole to All Orders in the Planck Length

Zhao

Zhang

et al. 2008

Int J Theor Phys

View full text Add to dashboard Cite

Using the quantum statistical method, the difficulty of solving the wave equation on the background of the black hole is avoided. We directly solve the partition functions of Bose and Fermi field on the background of an axisymmetric Kerr-Newman black hole using the new equation of state density motivated by the generalized uncertainty principle in the quantum gravity. Then near the black hole horizon, we calculate entropies of Bose and Fermi field between the black hole horizon surface and the hypersurface with the same inherent radiation temperature measured by an observer at an infinite distance. In our results there are not cutoffs and little mass approximation introduced in the conventional brick-wall method. The series expansion of the black hole entropy is obtained. And this series is convergent. It provides a way for studying the quantum statistical entropy of a black hole in a nonspherical symmetric spacetime.

show abstract

“…The geometric features of black hole temperature and entropy seem to imply that the black hole thermodynamics is closely related to nontrivial topological structure of spacetime. In [49] Cai, et al in order to relate the entropy with Euler characteristic χ of the corresponding Euclidean manifolds have been presented the following relation…”

Section: Resultsmentioning

confidence: 99%

The Cardy-Verlinde formula and entropyof topological Kerr- Newman black holes in de Sitter spaces

Setare

Altaie

2003

Eur. Phys. J. C

View full text Add to dashboard Cite

In this paper we show that the entropy of cosmological horizon in 4-dimensional Topological Kerr-Newman-de Sitter spaces can be described by the Cardy-Verlinde formula, which is supposed to be an entropy formula of conformal field theory in any dimension. Furthermore, we find that the entropy of black hole horizon can also be rewritten in terms of the Cardy-Verlinde formula for these black holes in de Sitter spaces, if we use the definition due to Abbott and Deser for conserved charges in asymptotically de Sitter spaces. Such result presume a well-defined dS/CFT correspondence, which has not yet attained the credibility of its AdS analogue. *

show abstract

Action and entropy of black holes in spacetimes with a cosmological constant

Cited by 88 publications

References 24 publications

Thermodynamics of de Sitter black holes with a conformally coupled scalar field

Thermodynamics of de Sitter black holes with a conformally coupled scalar field

Entropy of Kerr-Newman Black Hole to All Orders in the Planck Length

The Cardy-Verlinde formula and entropyof topological Kerr- Newman black holes in de Sitter spaces

Contact Info

Product

Resources

About