PARTITION FUNCTION OF THE REISSNER–NORDSTRÖM BLACK HOLE

We consider a microscopic model of a stretched horizon of the Reissner–Nordström black hole. In our model, the stretched horizon consists of discrete constituents. Using our model we obtain an explicit, analytic expression for the partition function of the hole. Our partition function implies, among other things, the Hawking effect, and provides it with a microscopic explanation as a phase transition taking place at the stretched horizon. The partition function also implies the Bekenstein–Hawking entropy law. The model and its consequences are similar to those obtained previously for the Schwarzschild black hole.

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Phase transition of quantum-corrected Schwarzschild black hole

Physics Letters B ◽

10.1016/j.physletb.2012.11.017 ◽

2012 ◽

Vol 718 (2) ◽

pp. 687-691 ◽

Cited By ~ 42

Author(s):

Wontae Kim ◽

Yongwan Kim

Keyword(s):

Phase Transition ◽

Black Hole ◽

Schwarzschild Black Hole

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SIGNATURES OF AN EMERGENT GRAVITY FROM BLACK HOLE ENTROPY

International Journal of Modern Physics D ◽

10.1142/s0218271809016156 ◽

2009 ◽

Vol 18 (14) ◽

pp. 2323-2327

Author(s):

CENALO VAZ

Keyword(s):

Phase Transition ◽

Black Hole ◽

Mass Spectrum ◽

Partition Function ◽

Ground State ◽

Degrees Of Freedom ◽

Thermodynamic Description ◽

Black Hole Entropy ◽

Fundamental Particle ◽

Horizon Radius

The existence of a thermodynamic description of horizons indicates that space–time has a microstructure. While the "fundamental" degrees of freedom remain elusive, quantizing Einstein's gravity provides some clues about their properties. A quantum AdS black hole possesses an equispaced mass spectrum, independent of Newton's constant, G, when its horizon radius is large compared to the AdS length. Moreover, the black hole's thermodynamics in this limit is inextricably connected with its thermodynamics in the opposite (Schwarzschild) limit by a duality of the Bose partition function. G, absent in the mass spectrum, re-emerges in the thermodynamic description through the Schwarzschild limit, which should be viewed as a natural "ground state." It seems that the Hawking–Page phase transition separates fundamental, "particle-like" degrees of freedom from effective, "geometric" ones.

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MICROSCOPIC BLACK HOLE AND UNCERTAINTY PRINCIPLE WITH MINIMAL LENGTH AND MOMENTUM

International Journal of Modern Physics A ◽

10.1142/s0217751x13500292 ◽

2013 ◽

Vol 28 (10) ◽

pp. 1350029 ◽

Cited By ~ 4

Author(s):

M. M. STETSKO

Keyword(s):

Phase Transition ◽

Heat Capacity ◽

Black Hole ◽

Uncertainty Principle ◽

Emission Rate ◽

Generalized Uncertainty Principle ◽

Minimal Length ◽

Schwarzschild Black Hole ◽

Evaporation Time ◽

Thermodynamical Functions

We investigate a microscopic black hole in the case of modified generalized uncertainty principle with a minimal uncertainty in position as well as in momentum. We calculate thermodynamical functions of a Schwarzschild black hole such as temperature, entropy and heat capacity. It is shown that the incorporation of minimal uncertainty in momentum leads to minimal temperature of a black hole. Minimal temperature gives rise to appearance of a phase transition. Emission rate equation and black hole's evaporation time are also obtained.

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Correlation loss and multipartite entanglement across a black hole horizon (

Quantum Information and Computation ◽

10.26421/qic9.7-8-8 ◽

2009 ◽

Vol 9 (7&8) ◽

pp. 657-665

Author(s):

G. Adesso ◽

I. Fuentes-Schuller

Keyword(s):

Black Hole ◽

Small Mass ◽

Point Of View ◽

Multipartite Entanglement ◽

Squeezed State ◽

Schwarzschild Black Hole ◽

Bipartite Entanglement ◽

Hawking Effect ◽

Entanglement Distribution ◽

Quantum And Classical Correlations

We investigate the Hawking effect on entangled fields. By considering a scalar field which is in a two-mode squeezed state from the point of view of freely falling (Kruskal) observers crossing the horizon of a Schwarzschild black hole, we study the degradation of quantum and classical correlations in the state from the perspective of physical (Schwarzschild) observers confined outside the horizon. Due to monogamy constraints on the entanglement distribution, we show that the lost bipartite entanglement is recovered as multipartite entanglement among modes inside and outside the horizon. In the limit of a small-mass black hole, no bipartite entanglement is detected outside the horizon, while the genuine multipartite entanglement interlinking the inner and outer regions grows infinitely.

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Maxwell’s Equal Area Law and the Hawking-Page Phase Transition

Journal of Gravity ◽

10.1155/2013/525696 ◽

2013 ◽

Vol 2013 ◽

pp. 1-7 ◽

Cited By ~ 21

Author(s):

Euro Spallucci ◽

Anais Smailagic

Keyword(s):

Phase Transition ◽

Heat Capacity ◽

Black Hole ◽

Critical Temperature ◽

Equation Of State ◽

Schwarzschild Black Hole ◽

Pure Radiation ◽

Equal Area ◽

Gravity Duality ◽

Area Law

We study the phases of a Schwarzschild black hole in the Anti-deSitter background geometry. Exploiting fluid/gravity duality, we construct the Maxwell equal area isotherm in the temperature-entropy plane, in order to eliminate negative heat capacity BHs. The construction we present here is reminiscent of the isobar cut in the pressure-volume plane which eliminates unphysical part of the Van der Walls curves below the critical temperature. Our construction also modifies the Hawking-Page phase transition. Stable BHs are formed at the temperature , while pure radiation persists for . turns out to be below the standard Hawking-Page temperature and there are no unstable BHs as in the usual scenario. Also, we show that, in order to reproduce the correct BH entropy , one has to write a black hole equation of state, that is, , in terms of the geometrical volume .

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Thermodynamic Relations for Kiselev and Dilaton Black Hole

Advances in High Energy Physics ◽

10.1155/2015/124910 ◽

2015 ◽

Vol 2015 ◽

pp. 1-11 ◽

Cited By ~ 2

Author(s):

Bushra Majeed ◽

Mubasher Jamil ◽

Parthapratim Pradhan

Keyword(s):

Phase Transition ◽

Black Holes ◽

Black Hole ◽

Phase Transitions ◽

Surface Temperature ◽

Schwarzschild Black Hole ◽

Event Horizons ◽

First Law Of Thermodynamics ◽

Special Cases ◽

Dilaton Black Hole

We investigate the thermodynamics and phase transition for Kiselev black hole and dilaton black hole. Specifically we consider Reissner-Nordström black hole surrounded by radiation and dust and Schwarzschild black hole surrounded by quintessence, as special cases of Kiselev solution. We have calculated the products relating the surface gravities, surface temperatures, Komar energies, areas, entropies, horizon radii, and the irreducible masses at the Cauchy and the event horizons. It is observed that the product of surface gravities, product of surface temperature, and product of Komar energies at the horizons are not universal quantities for the Kiselev solutions while products of areas and entropies at both the horizons are independent of mass of the above-mentioned black holes (except for Schwarzschild black hole surrounded by quintessence). For charged dilaton black hole, all the products vanish. The first law of thermodynamics is also verified for Kiselev solutions. Heat capacities are calculated and phase transitions are observed, under certain conditions.

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ASYMPTOTIC QUASINORMAL MODES OF d-DIMENSIONAL SCHWARZSCHILD BLACK HOLE WITH GAUSS–BONNET CORRECTION

International Journal of Modern Physics A ◽

10.1142/s0217751x06031612 ◽

2006 ◽

Vol 21 (17) ◽

pp. 3565-3574 ◽

Cited By ~ 17

Author(s):

SAYAN K. CHAKRABARTI ◽

KUMAR S. GUPTA

Keyword(s):

Black Hole ◽

Quasinormal Modes ◽

Quasinormal Mode ◽

Minimum Length ◽

Length Scale ◽

Schwarzschild Black Hole ◽

Analytic Expression ◽

Models Of Gravity ◽

Minimum Length Scale ◽

Bonnet Term

We obtain an analytic expression for the highly damped asymptotic quasinormal mode frequencies of the (d ≥ 5)-dimensional Schwarzschild black hole modified by the Gauss–Bonnet term, which appears in string derived models of gravity. The analytic expression is obtained under the string inspired assumption that there exists a minimum length scale in the system and in the limit when the coupling in front of the Gauss–Bonnet term in the action is small. Although there are several similarities of this geometry with that of the Schwarzschild black hole, the asymptotic quasinormal mode frequencies are quite different. In particular, the real part of the asymptotic quasinormal frequencies for this class of single horizon black holes is not proportional to log (3).

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