Modified entropy of Kerr-de Sitter black hole in Lorentz symmetry violation theory

Laxmi, Y. Onika; Singh, T. Ibungochouba; Meitei, I. Ablu

doi:10.1007/s10714-022-02954-z

Cited by 9 publications

(2 citation statements)

References 118 publications

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“…However, some calculations of the Hawking radiation, including the quantum tunneling approach, lead to the double Hawking problem [1,2,[11][12][13], where the obtained radiation is thermal but with temperature T = 2T H . We consider this problem in the semiclassical tunneling approach using the Klein-Gordon equation for a massive field in a curved background [11], which leads to the relativistic Hamilton-Jacobi equation for the classical action:…”

Section: T H Problem For Black Holesmentioning

confidence: 99%

“…Here, S BH = 4πM 2 G is the entropy of the black hole, and S WH = −4πM 2 G is the entropy of the white hole with the same mass. The latter is obtained from Equation (13). Since the tunneling transition can be considered as quantum fluctuation, the exponent in the tunneling process can be expressed as the difference between the entropies of the initial state (black hole) and the final state (white hole) [19].…”

Section: T H Problem For White Holesmentioning

confidence: 99%

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Double Hawking Temperature: From Black Hole to de Sitter

Volovik

2022

Universe

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The double Hawking temperature T=2TH appears in some approaches to the Hawking radiation when the radiation is considered in terms of the quantum tunneling. We consider the origin of such unusual temperature for the black hole horizon and also for the cosmological horizon in de Sitter spacetime. In the case of the black hole horizon, there are two contributions to the tunneling process of radiation, each being governed by the temperature T=2TH. These processes are coherently combined to produce the radiation with the Hawking temperature TH. This can be traditionally interpreted as the pair creation of two entangled particles, of which one goes towards the center of the black hole, while the other one escapes from the black hole. In the case of the cosmological horizon, the temperature T=2TH is physical. While the creation of the entangled pair is described by the Hawking temperature, the de Sitter spacetime allows for another process, in which only a single (non-entangled) particle inside the cosmological horizon is created. This process is characterized by the local temperature T=2TH. The local single-particle process also takes place outside the black hole horizon, but it is exponentially suppressed.

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Section: T H Problem For Black Holesmentioning

confidence: 99%

Section: T H Problem For White Holesmentioning

confidence: 99%

Double Hawking Temperature: From Black Hole to de Sitter

Volovik

2022

Universe

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Correction of Lorentz breaking theory to quantum tunneling radiation and entropy of black hole in gravity’s rainbow

Tan,

Zhang,

2023

Phys. Scr.

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Considering the Lorentz breaking theory, the correct modified forms of the dynamic equations of bosons and fermions in curved space-time can be studied. For the new form of fermions dynamic equation through spin 1/2 Dirac particles in the black hole space-time in gravity’s rainbow, by introducing aether-like vector field and correctly constructing gamma matrix, new meaningful expressions of Hawking temperature, tunneling rate and Bekenstein-Hawking entropy of this black hole are obtained. In addition, the distribution characteristics of the energy levels of Dirac particles are also studied, and meaningful results are obtained. The research results show that the Lorentz breaking terms will cause a certain degree of correction to the tunneling radiation of fermions in the curved space-time of the black hole.

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Maxwell's equal area law for Vaidya-Bonner-de Sitter black hole under Lorentz invariance violation

Singh,

Singh

2024

Chinese Phys. C

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In this study, we investigate the tunneling of fermions with arbitrary spin near the event horizon of a nonstationary Vaidya-Bonner-de Sitter (VBdS) black hole under Lorentz invariance violation (LIV). The modified Hawking temperature of VBdS black holes is calculated by using tortoise coordinate transformation, Feynman prescription, and Wentzel–Kramers–Brillouin approximation. By considering the cosmological constant as a thermodynamic pressure in the extended phase space, we construct a Maxwell's equal area law under LIV and study the phase transitions of VBdS black hole in , , and planes. The LIV increases the length of the liquid-gas coexistence region. The thermodynamic quantities such as the entropy, heat capacity, Helmholtz free energy, internal energy, enthalpy, and Gibbs free energy of the VBdS black hole are discussed. These quantities tend to increase under LIV. The stability of the black hole is also discussed in the presence of LIV.

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Modified entropy of Kerr-de Sitter black hole in Lorentz symmetry violation theory

Cited by 9 publications

References 118 publications

Double Hawking Temperature: From Black Hole to de Sitter

Double Hawking Temperature: From Black Hole to de Sitter

Correction of Lorentz breaking theory to quantum tunneling radiation and entropy of black hole in gravity’s rainbow

Maxwell's equal area law for Vaidya-Bonner-de Sitter black hole under Lorentz invariance violation

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