Near-horizon local instability and quantum thermality

Dalui, Surojit; Majhi, Bibhas Ranjan

doi:10.1103/physrevd.102.124047

Cited by 31 publications

(17 citation statements)

References 41 publications

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“…In the original work [17], the thermal nature of the Hawking effect is realized through the usage of Bogoliubov transformation between the ingoing and outgoing field modes described in terms of the null coordinates. The Hawking effect can be realized through other various means, like using tunnelling formalism [54][55][56][57][58][59][60], path integral approach [61], conformal symmetry [62], via anomalies [63][64][65], canonical formulation [66][67][68][69], and as an effect of near horizon local instability [70][71][72]. However, the conclusion remains the same, i.e., an asymptotic observer will perceive the BH horizon with some temperature proportional to its surface gravity.…”

Section: Hawking Effect In Radially Deformed Spacetimementioning

confidence: 99%

Thermal behavior of a radially deformed black hole spacetime

Barman

Mukherjee

2021

Eur. Phys. J. C

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In the present article, we study the Hawking effect and the bounds on greybody factor in a spacetime with radial deformation. This deformation is expected to carry the imprint of a non-Einsteinian theory of gravity, but shares some of the important characteristics of general relativity (GR). In particular, this radial deformation will restore the asymptotic behavior, and also allows for the separation of the scalar field equation in terms of the angular and radial coordinates – making it suitable to study the Hawking effect and greybody factors. However, the radial deformation would introduce a change in the locations of the horizon, and therefore, the temperature of the Hawking effect naturally alters. In fact, we observe that the deformation parameter has an enhancing effect on both temperature and bounds on the greybody factor, which introduces a useful distinction with the Kerr spacetime. We discuss these effects elaborately, and broadly study the thermal behavior of a radially deformed spacetime.

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Section: Hawking Effect In Radially Deformed Spacetimementioning

confidence: 99%

Thermal behavior of a radially deformed black hole spacetime

Barman

Mukherjee

2021

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…In the original work [17], the thermal nature of the Hawking effect is realized through the usage of Bogoliubov transformation between the ingoing and outgoing field modes described in terms of the null coordinates. The Hawking effect can be realized through other various means, like using tunnelling formalism [49][50][51][52][53][54][55], path integral approach [56], conformal symmetry [57], via anomalies [58][59][60], canonical formulation [61][62][63][64], and as an effect of near horizon local instability [65][66][67]. However, the conclusion remains the same, i.e., an asymptotic observer will perceive the BH horizon with some temperature proportional to its surface gravity.…”

Section: Hawking Effect In Radially Deformed Spacetimementioning

confidence: 99%

Thermal behavior of a radially deformed black hole spacetime

Barman¹,

Mukherjee²

2021

Preprint

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In the present article, we study the Hawking effect and the bounds on greybody factor in a spacetime with radial deformation. This deformation is expected to carry the imprint of a non-Einsteinian theory of gravity, but shares some of the important characteristics of general relativity (GR). In particular, this radial deformation will restore the asymptotic behavior, and also allows for the separation of the scalar field equation in terms of the angular and radial coordinates -making it suitable to study the Hawking effect and greybody factors. However, the radial deformation would introduce a change in the locations of the horizon, and therefore, the temperature of the Hawking effect naturally alters. In fact, we observe that the deformation parameter has an enhancing effect on both temperature and bounds on the greybody factor, which introduces a useful distinction with the Kerr spacetime. We discuss these effects elaborately, and broadly study the thermal behavior of a radially deformed spacetime.

show abstract

“…Nowadays, with the development of research in this respect, black hole, an unique thermodynamic system, presents incredible and peculiar thermodynamic properties with some quantum characteristics, such as Hawking-Page phase transition [14] corresponding to confinement-deconfinement transition in gauge theory [15] with the AdS/CFT correspondence, large and small black hole phase transition similar to gas-liquid phase transition [16][17][18][19][20][21], information loss of black hole [22], chaotic effect [23][24][25][26][27][28][29], and etc. Some phenomenological schemes have been proposed to analyze the thermodynamic properties of black holes.…”

Section: Introductionmentioning

confidence: 99%

Fokker-Planck equation for black holes in thermal potential

2021

Preprint

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We construct a kind of thermal potential and then put the black hole thermodynamic system in it. In this regard, some thermodynamic properties of the black hole are related to the geometric characteristics of the thermal potential. Driven by the intrinsic thermodynamic fluctuations, the behavior of the black hole in the thermal potential is stochastic. With the help of solving the Fokker-Planck equation analytically, we obtain the discrete energy spectrum of Schwarzschild and Banados-Teitelboim-Zanelli (BTZ) black holes in the thermal potential. For Schwarzschild black hole, the energy spectrum is proportional to the temperature of the ensemble, which is an external parameter, and the ground state is non-zero. For BTZ black hole, the energy spectrum only depends on the AdS radius, which is the intrinsic parameter. Moreover, the ground state of BTZ black hole in thermal potential is zero. This also reflects the difference between three-dimensional gravity and four-dimensional gravity.

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Near-horizon local instability and quantum thermality

Cited by 31 publications

References 41 publications

Thermal behavior of a radially deformed black hole spacetime

Thermal behavior of a radially deformed black hole spacetime

Thermal behavior of a radially deformed black hole spacetime

Fokker-Planck equation for black holes in thermal potential

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