Quasinormal modes and Hawking radiation of a Reissner-Nordström black hole surrounded by quintessence

Saleh, Mahamat; Bouetou, Bouetou Thomas; Kofané, Timoléon Crépin

doi:10.1007/s10509-011-0643-8

Cited by 43 publications

(20 citation statements)

References 27 publications

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“…To describe tunneling as an across horizon phenomena, it is necessary to choose coordinates which, unlike Schwarzschild coordinates, are not singular at the event horizon. Thus we rescale the time coordinate into Eddington-Finkelstein coordinates as t = T ± r * , where the + and − represent ingoing and outgoing particles respectively 39,40 . The tortoise coordinate r * is defined as,…”

Section: Hawking Radiation Via Tunnelingmentioning

confidence: 99%

Phase transition, quasinormal modes and Hawking radiation of Schwarzschild black hole in quintessence field

Tharanath

Varghese

Kuriakose³

2014

Mod. Phys. Lett. A

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Black hole thermodynamic stability can be determined by studying the nature of heat capacity of the system. For Schwarzschild black hole the heat capacity is negative, but in the quintessence field this system shows a second order phase transition, implying the existence of a stable phase. We further discuss the equation of state of the present system. While analyzing the quasinormal modes, we find that the massive scalar quasinormal mode frequencies in the complex ω plane shows a dramatic change when we plot it as a progressive function of quintessence state parameter. We also find the Hawking temperature of the system via the method of tunneling.

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Section: Hawking Radiation Via Tunnelingmentioning

confidence: 99%

Phase transition, quasinormal modes and Hawking radiation of Schwarzschild black hole in quintessence field

Tharanath

Varghese

Kuriakose³

2014

Mod. Phys. Lett. A

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“…This solution is a generalization of the Kiselev solution [53] to the charged case and its interesting properties are studied in [60][61][62][63]. Then, the generalized Kiselev solution is a subclass of our general dynamical solution (22) in the stationary limit.…”

Section: Surrounded Evaporating-accreting Bonnor-vaidya Black Hole Somentioning

confidence: 97%

Surrounded Bonnor–Vaidya solution by cosmological fields

Heydarzade

Darabi

2018

Eur. Phys. J. C

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In the present work, we generalize our previous work (Heydarzade and Darabi in arXiv:1710.04485, 2018 on the surrounded Vaidya solution by cosmological fields to the case of Bonnor-Vaidya charged solution. In this regard, we construct a solution for the classical description of the evaporating-accreting charged Bonnor-Vaidya black holes in the generic dynamical backgrounds. We address some interesting features of these solutions and classify them according to their behaviors under imposing the positive energy condition. Also, we analyze the timelike geodesics associated with the obtained solutions and show that some new correction terms arise in comparison to the case of standard Schwarzschild black hole. Then, we explore all these features for each of the cosmological backgrounds of dust, radiation, quintessence and cosmological constant-like fields in more detail.

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“…The rotating counterpart of Kiselev solution has been also obtained [27,28]. The thermodynamics of black holes in the quintessence background has been also investigated [29][30][31][32], and so is the quasinormal modes [33][34][35].…”

Section: Introductionmentioning

confidence: 99%

Black string surrounded by a static anisotropic quintessence fluid

2020

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A black string is a solution of the four-dimensional general relativity in cylindrical symmetric anti-de Sitter (AdS) spacetime pioneered by Lemos [6]. We obtain an exact rotating black string surrounded by quintessence matter in anti-de Sitter (AdS) spacetime and analyze its properties.The solution has an additional parameter N q due to background quintessence matter and it also depends on quintessence state parameter w q . Our rotating solution encompasses the Lemos black string [6], which can be recovered in the absence of background matter (N q = 0). The special case of rotating charged black string (w q = 1/3) has both Cauchy and event horizons. We find that thermodynamic quantities mass, temperature, entropy and heat capacity get corrected due to quintessence background. The counterterm method is utilized to calculate the associated conserved quantities to conclude that the first law of thermodynamics is satisfied. The cloud of strings background (w q = −1/3) has been included as a special case.

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Quasinormal modes and Hawking radiation of a Reissner-Nordström black hole surrounded by quintessence

Cited by 43 publications

References 27 publications

Phase transition, quasinormal modes and Hawking radiation of Schwarzschild black hole in quintessence field

Phase transition, quasinormal modes and Hawking radiation of Schwarzschild black hole in quintessence field

Surrounded Bonnor–Vaidya solution by cosmological fields

Black string surrounded by a static anisotropic quintessence fluid

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