scholarly journals Black holes in de Sitter space: Masses, energies, and entropy bounds

2004 ◽  
Vol 69 (6) ◽  
Author(s):  
Alejandro Corichi ◽  
Andres Gomberoff
Keyword(s):  
Black Holes ◽  
De Sitter Space ◽  
De Sitter ◽  
Entropy Bounds

scholarly journals Phase Transition and Entropy Force between Two Horizons in (n+2)-Dimensional de Sitter Space

2020 ◽  
Vol 2020 ◽  
pp. 1-8
Author(s):  
Yang Zhang ◽  
Wen-qi Wang ◽  
Yu-bo Ma ◽  
Jun Wang
Keyword(s):  
Phase Transition ◽  
Black Holes ◽  
Physical Mechanism ◽  
De Sitter Space ◽  
Space Time ◽  
Thermodynamic Quantities ◽  
De Sitter ◽  
Time Dimension ◽  
Cosmic Expansion

In this paper, the effect of the space-time dimension on effective thermodynamic quantities in (n+2)-dimensional Reissner-Nordstrom-de Sitter space has been studied. Based on derived effective thermodynamic quantities, conditions for the phase transition are obtained. The result shows that the accelerating cosmic expansion can be attained by the entropy force arisen from the interaction between horizons of black holes and our universe, which provides a possible way to explain the physical mechanism for the accelerating cosmic expansion.

scholarly journals Anti-de Sitter space and black holes

1998 ◽  
Vol 15 (11) ◽  
pp. 3575-3598 ◽  
Author(s):  
Máximo Bañados ◽  
Andrés Gomberoff ◽  
Cristián Martínez
Keyword(s):  
Black Holes ◽  
De Sitter Space ◽  
De Sitter

A de-Sitter weak gravity conjecture

2021 ◽  
Author(s):  
Ignatios Antoniadis ◽  
Karim Benakli
Keyword(s):  
Black Holes ◽  
Mass Formula ◽  
Flat Space ◽  
De Sitter Space ◽  
Large Radius ◽  
De Sitter ◽  
Time Result ◽  
A Charge ◽  
Weak Gravity ◽  
Charge Formula

The study of de-Sitter Reissner–Nordstrøm black holes allows us to uncover a Weak Gravity Conjecture in de-Sitter space. It states that for a given mass [Formula: see text] there should be a state with a charge [Formula: see text] bigger than a minimal value [Formula: see text], depending on the mass and the de-Sitter radius [Formula: see text], in Planck units. This reproduces the well-known flat space–time result [Formula: see text] in the large radius limit (large [Formula: see text]). In the highly curved de-Sitter space, ([Formula: see text]) [Formula: see text] behaves as [Formula: see text]. Finally, we discuss the case of backgrounds from gauged R-symmetry in [Formula: see text] supergravity. This paper is based on [I. Antoniadis and K. Benakli, Fortsch. Phys. 68, 2000054 (2020), arXiv:2006.12512 [hep-th]].

THERMODYNAMICS OF de SITTER SPACE–TIME IN YORK'S FORMALISM

2001 ◽  
Vol 16 (23) ◽  
pp. 1487-1492 ◽  
Author(s):  
BO-BO WANG ◽  
CHAO-GUANG HUANG
Keyword(s):  
Black Holes ◽  
Cosmological Constant ◽  
Path Integral ◽  
De Sitter Space ◽  
Space Time ◽  
Integral Approach ◽  
De Sitter ◽  
First Law Of Thermodynamics ◽  
Path Integral Approach ◽  
Thermodynamics Of Black Holes

The York's formalism of path-integral approach to the thermodynamics of black holes is applied to de Sitter space–time. The first law of thermodynamics for de Sitter space–time is given, which includes a "work term" with respect to the cosmological constant.

scholarly journals Abundant Stable Gauge Field Hair for Black Holes in Anti–de Sitter Space

2008 ◽  
Vol 100 (1) ◽  
Author(s):  
J. E. Baxter ◽  
Marc Helbling ◽  
Elizabeth Winstanley
Keyword(s):  
Black Holes ◽  
Gauge Field ◽  
De Sitter Space ◽  
De Sitter

scholarly journals NONSPHERICAL COLLAPSE OF TWO-FLUID STAR

2008 ◽  
Vol 23 (25) ◽  
pp. 4245-4254 ◽  
Author(s):  
S. G. GHOSH
Keyword(s):  
Black Holes ◽  
Equation Of State ◽  
Naked Singularity ◽  
De Sitter Space ◽  
Cosmic Censorship ◽  
De Sitter ◽  
Plane Symmetric ◽  
Cylindrically Symmetric ◽  
Hoop Conjecture ◽  
Two Fluid

We obtain the analog of collapsing Vaidya-like solution to include both a null fluid and a string fluid, with a linear equation of state (p⊥ = kρ), in nonspherical (plane symmetric and cylindrically symmetric) anti-de Sitter space–times. It turns out that the nonspherical collapse of two fluid in anti-de Sitter space–times, in accordance with cosmic censorship, proceed to form black holes, i.e. on naked singularity ever forms, in accordance with cosmic censorship, violating hoop conjecture.

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