Hawking radiation of the Vaidya–Bonner–de Sitter black hole

Chen, Deyou; Yang, Sijia

doi:10.1088/1367-2630/9/8/252

Cited by 25 publications

(19 citation statements)

References 22 publications

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“…r + − M r 2 + + a 2 + l 2 (19) this is consistent with the results derived from other methods. By using WKB approximation, the tunneling rate and the radiation spectrum of the emitted particle can be obtained.…”

Section: The Hamilton-jacobi Ansatzsupporting

confidence: 91%

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A New Method to Study the Hawking Radiation from the Kerr-NUT Black Hole

Liu

Hou

et al. 2008

Int J Theor Phys

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Developing Hamilton-Jacobi method, we discuss the Hawking radiation of Kerr-NUT black hole by considering the self-gravitation interaction as well as the energy conservation and angular momentum conservation. The result shows that the factual spectrum deviates from the precisely thermal one and the tunneling rate is related to the change of Bekenstein-Hawking entropy, which is accordant with that obtained by Parikh and Wilczek's method and gives an interesting correction to the Hawking radiation of the black hole.

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Section: The Hamilton-jacobi Ansatzsupporting

confidence: 91%

“…In the same year, a different method was introduced to calculate the imaginary part of the action given by Angheben et al [16][17][18][19][20]. The difference from Parikh's is mainly that such method concentrates on introducing the proper spatial distance and upon calculating the relativistic Hamilton-Jacobi equation.…”

Section: Introductionmentioning

confidence: 99%

A New Method to Study the Hawking Radiation from the Kerr-NUT Black Hole

Liu

Hou

et al. 2008

Int J Theor Phys

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“…Up to now, a lot of work has already been successfully carried out for further extension of the quantum tunneling method [19][20][21][22][23][24][25][26][27][28]. But most of them are limited to investigate the scalar particles radiation.…”

Section: Introductionmentioning

confidence: 99%

Fermion tunneling from a non-static black hole with the internal global monopole

Cai

Lin

2009

Gen Relativ Gravit

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Kerner and Mann's recent research shows that the Hawking temperature and tunneling rate can be obtained by the fermion tunneling method from the Rindler space-time and a general non-rotating black hole. In this paper, considering the tunneling particles with spin 1/2 and taking into account the particle's self-gravitation in the dynamical background space-time, we further improve Kerner and Man's fermion tunneling method to investigate Hawking radiation via tunneling from a non-static black hole with the internal global monopole. The result shows that the tunneling rate of the non-static black hole is related to the integral of the changing horizon besides the change of Bekenstein-Hawking entropy, which is different from the stationary cases. It also essentially implies that the unitary is violated for the reason that the black hole is non-stationary and cannot be treated as an isolated system.

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“…Farmany ( ) Young Researchers Club, Hamedan Branch, Islamic Azad University, For example, in each static or stationary space time k is just the surface gravity of the horizon, but in the VaidyaBonner-de Sitter space time, it is no longer the surface gravity of event horizon and the cosmic horizon. This property makes the Vaidya-Bonner solution as an important horizon (Chen and Yang 2007;Liu et al 2003;Li and Zhao 2001;Lin and Yang 2009;Zhou and Liu 2009;Li et al 1999;Niu and Liu 2010). In this letter, we calculate the entropy of the Vaidya-Bonner-de Sitter space time.…”

mentioning

confidence: 96%

“…This property makes the Vaidya-Bonner solution as an important horizon (Chen and Yang 2007;Liu et al 2003;Li and Zhao 2001;Lin and Yang 2009;Zhou and Liu 2009;Li et al 1999;Niu and Liu 2010). In this letter, we calculate the entropy of the Vaidya-Bonner-de Sitter space time.…”

mentioning

confidence: 96%

Thermodynamics of Vaidya-Bonner-de Sitter space time based on the generalized space-time uncertainty

Farmany

2011

Astrophys Space Sci

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In each static or stationary space time k is just surface gravity of the horizon, but in the of Vaidya-Bonnerde Sitter space time, it is no longer the surface gravity of the event horizon. This property makes the VaidyaBonner as an important horizon. In this paper, the entropy of Vaidya-Bonner-de Sitter space time is calculated. In continue, employing the generalized uncertainty principle, quantum gravitational corrections to the entropy of VaidyaBonner space time is studied.It is interesting that without calculating the energy-momentum tensor of evaporating black hole we calculate the temperature of its event horizon. The of Vaidya-Bonner-de Sitter calculation is the simple method that without calculating the vacuum expectation value of the renormalized energymomentum tensor, we can determine the horizon's temperature. In this scenario, the Klein-Gordon equation can be reduced to the standard form of wave equation in the tortoise coordinate of the Schwarzschild space time. However in a non-static space time Zheng-Dai approaches give the horizon's temperature. Recently this method have received much attention (Zheng and Xianxin 1992;Zheng et al. 1994;Damour and Ruffini 1976;Balbinot 1986;Hiscock 1981). On the other hand, some property of the Vaidya-Bonner space time differ it with other space times.A. Farmany ( ) Young Researchers Club, Hamedan Branch, Islamic Azad University, For example, in each static or stationary space time k is just the surface gravity of the horizon, but in the VaidyaBonner-de Sitter space time, it is no longer the surface gravity of event horizon and the cosmic horizon. This property makes the Vaidya-Bonner solution as an important horizon (Chen and Yang 2007;Liu et al. 2003;Li and Zhao 2001;Lin and Yang 2009;Zhou and Liu 2009;Li et al. 1999;Niu and Liu 2010). In this letter, we calculate the entropy of the Vaidya-Bonner-de Sitter space time. Let we begin with the Vaidya-Bonner-de Sitter solution,Where ς = 2m r + Q 2 r 2 + λr 2 3 and λ is the cosmological constant. Not that mass and charge are Eddington-Finkelstein time ν dependent. , Wanglin et al. (2007 the Hawking temperature of the Vaidya-Bonner-de Sitter event horizon is obtained from a solution to the surface gravity of this space time,The black hole entropy is usually derived from the Hawking temperature. Setting M to mean energy and T to mean temperature, the entropy may defined from the well-known thermodynamics relation as,Inserting (2) into (3), one find dM dS = r − m − 2 3 λr 2 − 2rṙ 2πK B ςr 2 (4)

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Hawking radiation of the Vaidya–Bonner–de Sitter black hole

Cited by 25 publications

References 22 publications

A New Method to Study the Hawking Radiation from the Kerr-NUT Black Hole

A New Method to Study the Hawking Radiation from the Kerr-NUT Black Hole

Fermion tunneling from a non-static black hole with the internal global monopole

Thermodynamics of Vaidya-Bonner-de Sitter space time based on the generalized space-time uncertainty

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