Higher dimensional black hole radiation and a generalized uncertainty principle

Dehghani, M.; Farmany, Abbas

doi:10.1016/j.physletb.2009.04.058

Cited by 32 publications

(39 citation statements)

References 45 publications

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“…The Heisenberg uncertainty principle can be generalized within the microphysics regime as [25,[29][30][31][32][33][37][38][39][40][41][42][43][44][45][46] x p ≥h…”

Section: The Fragmentation Of Black Hole With F (R) Global Monopole Umentioning

confidence: 99%

“…According to the combination of the GUP and the approximation (15), we estimate the black hole horizon amended by the gravitation with the original horizon of black hole as the lower bound on the region like x = 2r H [30][31][32][33]47,48],…”

Section: The Fragmentation Of Black Hole With F (R) Global Monopole Umentioning

confidence: 99%

“…The generalized uncertainty principle (GUP) with the additional terms can be used to cure the divergence from states density near the black hole horizon and relate the entropy of black hole to a minimal length as quantum gravity scale [30][31][32][33]. The influence from the GUP modifying the black hole horizon and definitely changing the black hole entropy further was considered in terms of the radiation from black holes [30][31][32][33].…”

Section: Introductionmentioning

confidence: 99%

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The fragmentation instability of a black hole with f(R) global monopole under GUP

Chen

Cheng

2018

Eur. Phys. J. C

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Having studied the fragmentation of the black holes containing f (R) global monopole under the generalized uncertainty principle (GUP), we show the influences from this kind of monopole, f (R) theory, and GUP on the evolution of black holes. We focus on the possibility that the black hole breaks into two parts by means of the second law of thermodynamics. We derive the entropies of the initial black hole and the broken parts while the generalization of Heisenberg's uncertainty principle is introduced. We find that the f (R) global monopole black hole keeps stable instead of splitting without the generalization because the entropy difference is negative. The fragmentation of the black hole will happen if the black hole entropies are limited by the GUP and the considerable deviation from the general relativity leads to the case that the mass of one fragmented black hole is smaller and the other one's mass is larger.

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“…The Heisenberg uncertainty principle can be generalized within the microphysics regime as [25,[29][30][31][32][33][37][38][39][40][41][42][43][44][45][46] x p ≥h…”

Section: The Fragmentation Of Black Hole With F (R) Global Monopole Umentioning

confidence: 99%

Section: The Fragmentation Of Black Hole With F (R) Global Monopole Umentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The fragmentation instability of a black hole with f(R) global monopole under GUP

Chen

Cheng

2018

Eur. Phys. J. C

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“…It is shown that usual uncertainty principle receives a modification at the microphysics regime (Witten 1996;Amati et al 1987;Yoneya 2000;Adler 1999;Hossenfelder et al 2004;Maggiore 1994;Farmany et al 2007Farmany et al , 2008Veneziano 1980;Kempf 1997;Hossenfelder et al 2003;Kempf and Managano 1997;Ali et al 2009Ali et al , 2011Das et al 2010;Dehghani and Farmany 2009a;Farmany 2006) x…”

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confidence: 99%

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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“…;Medved and Vage- nas 2005;Vagenas 2003;Arzano et al 2005;Kerner and Mann 2006;Akhmedov et al 2007;Criscienzo et al 2007;Farmany et al 2009;Dehghani and Farmany 2009; Baner- jee and Majhi 2008a, 2008b;Akhmedova et al 2008;Banerjee and Kulkarni 2008;Smailagic and Spallucci 2004).…”

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confidence: 99%

Semiclassical tunneling radiation of Kehagias-Sfetsos black hole and holographic principle

Farmany

2011

Astrophys Space Sci

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Higher dimensional black hole radiation and a generalized uncertainty principle

Cited by 32 publications

References 45 publications

The fragmentation instability of a black hole with f(R) global monopole under GUP

The fragmentation instability of a black hole with f(R) global monopole under GUP

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

Semiclassical tunneling radiation of Kehagias-Sfetsos black hole and holographic principle

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