scholarly journals Particle collisions near the cosmological horizon of a Reissner-Nordström-de Sitter black hole

JETP Letters ◽  
2011 ◽  
Vol 94 (8) ◽  
pp. 589-592 ◽  
Author(s):  
C. Zhong ◽  
S. Gao
Keyword(s):  
Black Hole ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Particle Collisions

scholarly journals LUKEWARM BLACK HOLES IN QUADRATIC GRAVITY

2011 ◽  
Vol 26 (14) ◽  
pp. 999-1007 ◽  
Author(s):  
JERZY MATYJASEK ◽  
KATARZYNA ZWIERZCHOWSKA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Event Horizon ◽  
Fourth Order ◽  
Spherically Symmetric ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Quadratic Gravity ◽  
De Sitter Universe ◽  
Electrically Charged

Perturbative solutions to the fourth-order gravity describing spherically-symmetric, static and electrically charged black hole in an asymptotically de Sitter universe is constructed and discussed. Special emphasis is put on the lukewarm configurations, in which the temperature of the event horizon equals the temperature of the cosmological horizon.

scholarly journals Existence condition and phase transition of Reissner–Nordström–de Sitter black hole

2014 ◽  
Vol 29 (09) ◽  
pp. 1450050 ◽  
Author(s):  
Meng-Sen Ma ◽  
Hui-Hua Zhao ◽  
Li-Chun Zhang ◽  
Ren Zhao
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Thermodynamic Properties ◽  
Electric Charge ◽  
Transition Point ◽  
Existence Condition ◽  
Phase Transition Point ◽  
Black Hole Horizon ◽  
Cosmological Horizon ◽  
De Sitter

After introducing the connection between the black hole horizon and the cosmological horizon, we discuss the thermodynamic properties of Reissner–Nordström–de Sitter (RN–dS) space–time. We present the condition under which RN–dS black hole can exist. Employing Ehrenfest' classification, we conclude that the phase transition of RN–dS black hole is the second-order one. The position of the phase transition point is irrelevant to the electric charge of the system. It only depends on the ratio of the black hole horizon and the cosmological horizon.

scholarly journals THE CARDY–VERLINDE FORMULA AND ENTROPY OF TOPOLOGICAL REISSNER–NORDSTRÖM BLACK HOLES IN DE SITTER SPACES

2002 ◽  
Vol 17 (32) ◽  
pp. 2089-2094 ◽  
Author(s):  
M. R. SETARE
Keyword(s):  
Field Theory ◽  
Black Holes ◽  
Black Hole ◽  
Conformal Field Theory ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Conformal Field ◽  
Entropy Formula ◽  
Verlinde Formula ◽  
Entropy Of Black Hole

In this paper we discuss the question of whether the entropy of cosmological horizon in topological Reissner–Nordström–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. Our result is in favour of the dS/CFT correspondence.

Tunneling Radiation from the Cosmological Horizon

2013 ◽  
Vol 647 ◽  
pp. 918-922
Author(s):  
Hui Ling Li ◽  
Cheng Cheng ◽  
Yan Ge Wu
Keyword(s):  
Black Hole ◽  
Hawking Radiation ◽  
Quantum Tunneling ◽  
Tunneling Rate ◽  
Real Spectrum ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Tunneling Radiation ◽  
Unitary Theory ◽  
The Real

Extending the Parikh’s method of quantum tunneling radiation, Hawking radiation via tunneling from the cosmological horizon of NUT-Kerr-Newman de Sitter black hole is deeply studied. The result shows that the tunneling rate on the cosmological horizon is related to the change of Bekenstein-Hawking entropy and the real spectrum is not strictly thermal at all, but is consistent with an underlying unitary theory.

scholarly journals Phase transitions and entropy force of charged de Sitter black holes with cloud of string and quintessence

2020 ◽  
Vol 29 (15) ◽  
pp. 2050108
Author(s):  
Yubo Ma ◽  
Yang Zhang ◽  
Ren Zhao ◽  
Shuo Cao ◽  
Tonghua Liu ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Phase Transitions ◽  
Black Hole Horizon ◽  
Thermodynamic Quantities ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Lennard Jones ◽  
First Order Phase Transition ◽  
First Order Phase

In this paper, we investigate the combined effects of the cloud of strings and quintessence on the thermodynamics of a Reissner–Nordström–de Sitter black hole. Based on the equivalent thermodynamic quantities considering the correlation between the black hole horizon and the cosmological horizon, we extensively discuss the phase transitions of the spacetime. Our analysis proves that similar to the case in AdS spacetime, second-order phase transitions could take place under certain conditions, with the absence of first-order phase transition in the charged de Sitter (dS) black holes with cloud of string and quintessence. The effects of different thermodynamic quantities on the phase transitions are also quantitatively discussed, which provides a new approach to study the thermodynamic qualities of unstable dS spacetime. Focusing on the entropy force generated by the interaction between the black hole horizon and the cosmological horizon, as well as the Lennard–Jones force between two particles, our results demonstrate the strong degeneracy between the entropy force of the two horizons and the ratio of the horizon positions, which follows the surprisingly similar law given the relation between the Lennard–Jones force and the ratio of two particle positions. Therefore, the study of the entropy force between two horizons is not only beneficial to the deep exploration of the three modes of cosmic evolution, but also helpful to understand the correlation between the microstates of particles in black holes and those in ordinary thermodynamic systems.

THE SCALAR FIELD IN EXTREME REISSNER–NORDSTRÖM–DE SITTER SPACE

2003 ◽  
Vol 18 (26) ◽  
pp. 4829-4836 ◽  
Author(s):  
GUANG-HAI GUO ◽  
YUAN-XING GUI ◽  
JIAN-XIANG TIAN
Keyword(s):  
Black Hole ◽  
Field Equation ◽  
Scalar Field ◽  
Special Interest ◽  
Field Amplitude ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Reflection And Transmission ◽  
Transmission Coefficients ◽  
Tortoise Coordinate

By generalizing the method of I. Brevik et al. the scalar field equation between the outer black hole horizon and the cosmological horizon in the extreme Reissner–Nordström–de Sitter (RNdS) geometry is solved. The field amplitude, as well as the potential, is shown graphically by introducing the "tangent" approximation, which is more exact than that used by I. Brevik et al., of the tortoise coordinate. There are two limiting cases of our special interest. The first one is when the cosmological horizon is very close to the outer horizon of the "black hole." The second one is when they are far apart. And the reflection and transmission coefficients are worked out in the two cases respectively.

scholarly journals The price of curiosity: information recovery in de Sitter space

2021 ◽  
Vol 2021 (5) ◽  
Author(s):  
Lars Aalsma ◽  
Watse Sybesma
Keyword(s):  
Black Hole ◽  
Thermal Equilibrium ◽  
De Sitter Space ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Information Recovery ◽  
Fine Grained ◽  
Black Hole Radiation ◽  
Entropy Of Black Hole

Abstract Recent works have revealed that quantum extremal islands can contribute to the fine-grained entropy of black hole radiation reproducing the unitary Page curve. In this paper, we use these results to assess if an observer in de Sitter space can decode information hidden behind their cosmological horizon. By computing the fine-grained entropy of the Gibbons-Hawking radiation in a region where gravity is weak we find that this is possible, but the observer’s curiosity comes at a price. At the same time the island appears, which happens much earlier than the Page time, a singularity forms which the observer will eventually hit. We arrive at this conclusion by studying de Sitter space in Jackiw-Teitelboim gravity. We emphasize the role of the observer collecting radiation, breaking the thermal equilibrium studied so far in the literature. By analytically solving for the backreacted geometry we show how an island appears in this out-of-equilibrium state.

scholarly journals Spacetime Entanglement Entropy of de Sitter and Black Hole Horizons

2021 ◽  
Author(s):  
Abhishek Mathur ◽  
Sumati Surya ◽  
Nomaan X
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Density Matrix ◽  
Mixed State ◽  
Entanglement Entropy ◽  
Spatial Density ◽  
De Sitter Spacetime ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Sitter Spacetime

Abstract We calculate Sorkin's manifestly covariant, spacetime entanglement entropy (SSEE) for a massive and massless minimally coupled free Gaussian scalar field for the de Sitter horizon and Schwarzschild de Sitter horizons, respectively, in d > 2. In de Sitter spacetime we restrict the Bunch-Davies vacuum in the conformal patch to the static patch to obtain a mixed state. The finiteness of the spatial L2 norm in the static patch implies that the SSEE is well defined for each mode. We find that for this mixed state it is independent of the effective mass of the scalar field and matches results obtained by Higuchi and Yamamoto, where, a spatial density matrix was used to calculate the horizon entanglement entropy. Using a cut-off in the angular modes we show that the SSEE is proportional to the area of the de Sitter cosmological horizon. Our analysis can be carried over to the black hole and cosmological horizon in Schwarzschild de Sitter spacetime, which also has finite spatial L2 norm in the static regions. Although the explicit form of the modes is not known in this case, we use appropriate boundary conditions for a massless minimally coupled scalar field, to find the mode-wise SSEE for both the black hole and de Sitter cosmological horizons. As in the de Sitter calculation we see that SSEE is proportional to the horizon area in each case after taking a cut-off in the angular modes.

scholarly journals On the duality of Schwarzschild-de Sitter spacetime and moving mirror

2022 ◽  
Author(s):  
Diego Fernández-Silvestre ◽  
Joshua Foo ◽  
Michael R.R Good
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Simple Solution ◽  
Particle Spectrum ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Einstein’S Equations ◽  
Relative Temperature ◽  
Einstein's Equations ◽  
Sitter Spacetime

Abstract The Schwarzschild-de Sitter (SdS) metric is the simplest spacetime solution in general relativity with both a black hole event horizon and a cosmological event horizon. Since the Schwarzschild metric is the most simple solution of Einstein's equations with spherical symmetry and the de Sitter metric is the most simple solution of Einstein's equations with a positive cosmological constant, the combination in the SdS metric defines an appropriate background geometry for semi-classical investigation of Hawking radiation with respect to past and future horizons. Generally, the black hole temperature is larger than that of the cosmological horizon, so there is heat flow from the smaller black hole horizon to the larger cosmological horizon, despite questions concerning the definition of the relative temperature of the black hole without a measurement by an observer sitting in an asymptotically flat spacetime. Here we investigate the accelerating boundary correspondence (ABC) of the radiation in SdS spacetime without such a problem. We have solved for the boundary dynamics, energy flux and asymptotic particle spectrum. The distribution of particles is globally non-thermal while asymptotically the radiation reaches equilibrium.

scholarly journals Shocks and information exchange in de Sitter space

2021 ◽  
Vol 2021 (10) ◽  
Author(s):  
L. Aalsma ◽  
A. Cole ◽  
E. Morvan ◽  
J. P. van der Schaar ◽  
G. Shiu
Keyword(s):  
Black Hole ◽  
Information Exchange ◽  
Information Transfer ◽  
Recent Progress ◽  
Vacuum State ◽  
De Sitter Space ◽  
Cosmological Horizon ◽  
De Sitter ◽  
Black Hole Information ◽  
Selection Of

Abstract We discuss some implications of recent progress in understanding the black hole information paradox for complementarity in de Sitter space. Extending recent work by two of the authors, we describe a bulk procedure that allows information expelled through the cosmological horizon to be received by an antipodal observer. Generically, this information transfer takes a scrambling time t = H−1 log(SdS). We emphasize that this procedure relies crucially on selection of the Bunch-Davies vacuum state, interpreted as the thermofield double state that maximally entangles two antipodal static patches. The procedure also requires the presence of an (entangled) energy reservoir, created by the collection of Hawking modes from the cosmological horizon. We show how this procedure avoids a cloning paradox and comment on its implications.

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