Dying AdS Schwarzschild black hole

The criteria for thermal stability of a most general quantum black hole derived by us appeared in the form of a series of inequalities connecting second-order derivatives of black hole mass with respect to its parameters, which determine the mass of the black hole. These nullify the concept of positivity of specific heat as the sole criteria for thermal stability. Using this most general stability criterion, we prove here that AdS Schwarzschild black holes are no longer stable anywhere in their parameter space if cosmological constant is allowed to vary. We also calculate the fluctuations of both horizon area and cosmological constant of this black hole. We calculate specific heat of it and compare this with Hawking’s prediction.

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Thermodynamics of asymptotically flat Reissner–Nordstrom black hole

Modern Physics Letters A ◽

10.1142/s0217732321500711 ◽

2021 ◽

pp. 2150071

Author(s):

Aloke Kumar Sinha

Keyword(s):

Phase Transition ◽

Thermal Stability ◽

Black Holes ◽

Black Hole ◽

Black Hole Mass ◽

Schwarzschild Black Hole ◽

Asymptotically Flat ◽

Electrically Charged ◽

Derivatives Of ◽

Thermal Stability Of

We established the criteria for thermal stability of a most general black hole in the form of a series of inequalities connecting second-order derivatives of the black hole mass with respect to its parameters. The mass of a black hole depends solely on these parameters, e.g. horizon area and electric charge are these parameters for non-rotating charged black hole. We also introduced the notion of “Quasi stability”. It is known how to calculate the fluctuations of these parameters for both stable and quasi stable black holes. In this paper, we consider the simplest black hole having nontrivial parameter, i.e. electrically charged non-rotating asymptotically flat Reissner–Nordstrom black hole (AFRNBH). We will show here that this black hole is not stable anywhere in its parameter space, but it is actually quasi stable, having positive specific heat in some region, violating Hawking’s prediction. In fact, this black hole will be shown to exhibit phase transition which is structurally quite different from that in case of Schwarzschild black hole, as predicted first by Hawking. This black hole will also be shown to try to resist its decay under Hawking radiation, but ultimately remains unsuccessful.

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Fermion tunneling, Instability and First Law of Rindler Modified Schwarzschild Black Hole as a Thermodynamic system

Canadian Journal of Physics ◽

10.1139/cjp-2020-0027 ◽

2020 ◽

Author(s):

S. Fatemeh Mirekhtiary ◽

I. Sakalli ◽

V. Bashiry

Keyword(s):

Thermal Stability ◽

Black Hole ◽

Cosmological Constant ◽

Event Horizon ◽

Quantum Tunneling ◽

Thermodynamic System ◽

Unstable System ◽

Schwarzschild Black Hole ◽

Rindler Acceleration ◽

Thermal Stability Of

This study investigated quantum tunneling of spin half particles through the event horizon of Rindler modified Schwarzschild black hole (RMSBH) in the presence of quintessence matter. We analyzed the thermodynamics of RMSBH in the Kiselev coordinates. Particularly, exploring RMSBH's entropy and the thermal stability of the RMSBH. We showed that RMSBH serves an unstable system causing fluctuations. The integral formulation of the first law of RMSBH in the absence of cosmological constant was also represented. By using the first law, we finally studied the Ruppeiner geometry for Rindler acceleration and pressure with fixed ensembles .

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Phase transition in decaying black holes

Modern Physics Letters A ◽

10.1142/s0217732320502582 ◽

2020 ◽

Vol 35 (31) ◽

pp. 2050258

Author(s):

Aloke Kumar Sinha

Keyword(s):

Phase Transition ◽

Black Holes ◽

Black Hole ◽

Phase Transitions ◽

Quantum Black Hole ◽

Dimensional Spacetime ◽

The Stability ◽

Derivatives Of ◽

Physical Quantities ◽

Thermal Stability Of

We had earlier derived the most general criteria for thermal stability of a quantum black hole, with arbitrary number of parameters, in any dimensional spacetime. These conditions appeared in form of a series of inequalities connecting second order derivatives of black hole mass with respect to its parameters. Some black holes like asymptotically flat rotating charged black holes do not satisfy all the stability criteria simultaneously, but do satisfy some of them in certain region of parameter space. They are known as “Quasi Stable” black holes. In this paper, we will show that quasi stable black holes although ultimately decay under Hawking radiation undergo phase transitions. These phase transitions are different from phase transition in ADS Schwarzschild black hole. These are marked by sign changes in certain physical quantities apart from specific heat of the black hole. We will also discuss the changes in the nature of fluctuations of the parameters of these quasi stable black holes with different phases.

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Classical Soft Theorem in the AdS-Schwarzschild spacetime in small cosmological constant limit

Journal of High Energy Physics ◽

10.1007/jhep01(2021)038 ◽

2021 ◽

Vol 2021 (1) ◽

Author(s):

Nabamita Banerjee ◽

Arindam Bhattacharjee ◽

Arpita Mitra

Keyword(s):

Black Hole ◽

Cosmological Constant ◽

Mass Parameter ◽

Flat Space ◽

Leading Order ◽

Probe Particle ◽

Black Hole Mass ◽

Schwarzschild Black Hole ◽

Soft Factor ◽

Soft Limit

Abstract We have studied scattering of a probe particle by a four dimensional AdS-Schwarzschild black hole at large impact factor. Our analysis is consistent perturbatively to leading order in the AdS radius and black hole mass parameter. Next we define a proper “soft limit” of the radiation and extract out the “soft factor” from it. We find the correction to the well known flat space Classical Soft graviton theorem due to the presence of an AdS background.

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BEKENSTEIN-SPECTRUM, TEMPERATURE AND SPECIFIC HEAT OF BLACK HOLES FROM CHAINS

International Journal of Modern Physics A ◽

10.1142/s0217751x05024304 ◽

2005 ◽

Vol 20 (13) ◽

pp. 2813-2820 ◽

Cited By ~ 2

Author(s):

AXEL KRAUSE

Keyword(s):

Black Holes ◽

Black Hole ◽

Mass Spectrum ◽

Specific Heat ◽

Hawking Temperature ◽

Evaporation Process ◽

Black Hole Mass ◽

Schwarzschild Black Hole ◽

Discrete Mass

We study some consequences of a recently proposed description for a Schwarzschild black hole based on Euclidean [Formula: see text] brane pairs described in terms of chain-like excitations. A discrete mass-spectrum of Bekenstein-type is inferred and upon identification of the black hole mass with the chain's energy the leading corrections to both Hawking-temperature and specific heat of the black hole are obtained. The results indicate that for small black holes the evaporation process might be considerably altered.

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Preparation and Pyrolysis of Stereoisomeric Bromobicyclo[n.1.0]alkanes ( n = 6, 8 , 10)

Zeitschrift für Naturforschung B ◽

10.1515/znb-1987-0416 ◽

1987 ◽

Vol 42 (4) ◽

pp. 489-494 ◽

Cited By ~ 7

Author(s):

Eckehard V. Dehmlow ◽

Roland Kramer

Keyword(s):

Thermal Stability ◽

Gas Phase ◽

Condensed Phase ◽

Secondary Products ◽

Gas Phase Reactions ◽

Stereoselective Reduction ◽

Derivatives Of ◽

Thermal Stability Of

Abstract The title compounds la-3c were prepared by stereoselective reduction of the respective dibromides. Pyrolysis gave allylic bromides (8, 9, 11) as primary and dienes (10, 12) as secondary products. Product ratios were independent of the stereochemistry of the starting materials. No differences of the rearrangement rates of the stereoisomers were observed in gas phase reactions of the derivatives of bicyclo[6.1.0]- and bicyclo[8.1.0]alkanes. With the larger bicyclo[10.1.0] derivatives, however, distinct differences in the thermal stability of cis-trans-isomers4c/5c or 2c/3c were found in condensed phase.

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DE SITTER-SCHWARZSCHILD BLACK HOLE: ITS PARTICLELIKE CORE AND THERMODYNAMICAL PROPERTIES

International Journal of Modern Physics D ◽

10.1142/s0218271896000333 ◽

1996 ◽

Vol 05 (05) ◽

pp. 529-540 ◽

Cited By ~ 100

Author(s):

I.G. DYMNIKOVA

Keyword(s):

Black Hole ◽

Lower Limit ◽

Mass Parameter ◽

Hawking Temperature ◽

Einstein Equations ◽

Black Hole Mass ◽

De Sitter ◽

Schwarzschild Black Hole ◽

Schwarzschild Solution ◽

Second Order Phase Transition

We analyze the globally regular solution of the Einstein equations describing a black hole whose singularity is replaced by the de Sitter core. The de Sitter—Schwarzschild black hole (SSBH) has two horizons. Inside of it there exists a particlelike structure hidden under the external horizon. The critical value of mass parameter M cr1 exists corresponding to the degenerate horizon. It represents the lower limit for a black-hole mass. Below M cr1 there is no black hole, and the de Sitter-Schwarzschild solution describes a recovered particlelike structure. We calculate the Hawking temperature of SSBH and show that specific heat is broken and changes its sign at the value of mass M cr 2>M cr 1 which means that a second-order phase transition occurs at that point. We show that the Hawking temperature drops to zero when a mass approaches the lower limit M cr1 .

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