Quantum Corrections for a Bardeen Regular Black Hole

Sharif, M.; Javed, Wajiha

doi:10.3938/jkps.57.217

Cited by 49 publications

(35 citation statements)

References 20 publications

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“…where β is the monopole charge of a self-gravitating magnetic field described by a nonlinear electrodynamics source, and m is the mass of the black hole, the metric (1) reduces to the Bardeen regular black hole metric [32,[39][40][41]. Quintessence is a scalar field whose equation of state parameter, ω q , is defined as a ratio of its pressure, p, and its energy density, ρ [42].…”

Section: The Regular Bardeen Black Hole Surrounded By Quintessencementioning

confidence: 99%

Quasinormal modes of gravitational perturbation around regular Bardeen black hole surrounded by quintessence

2018

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In this paper, Quasinormal modes of gravitational perturbation are investigated for the regular Bardeen black hole surrounded by quintessence. Considering the metric of the Bardeen spacetime surrounded by quintessence, we derived the perturbation equation for gravitational perturbation using Regge-Wheeler gauge. The third order WentzelKramers-Brillouin (WKB) approximation method is used to evaluate quasinormal frequencies. Explicitly, the behaviors of the black hole potential and quasinormal modes were plotted. The results show that, due to the presence of quintessence, the gravitational perturbation around the black hole damps more slowly and oscillates more slowly.

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Section: The Regular Bardeen Black Hole Surrounded By Quintessencementioning

confidence: 99%

Quasinormal modes of gravitational perturbation around regular Bardeen black hole surrounded by quintessence

2018

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“…Furthermore, they analyzed the corresponding Hawking temperature of these BHs. Sharif and Javed [99] have also investigated the quantum corrections for regular BHs, i.e., Bardeen and ABGB.…”

Section: Introductionmentioning

confidence: 99%

Hawking radiation from cubic and quartic black holes via tunneling of GUP corrected scalar and fermion particles

2019

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We analyze the effect of the generalized uncertainty (GUP) principle on the Hawking radiation from the hairy black hole in U(1) gauge-invariant scalar-vector-tensor theory by utilizing the semiclassical Hamilton-Jacobi method. To do so, we evaluate the tunneling probabilities and Hawking temperature for scalar and fermion particles for the given spacetime of the black holes with cubic and quartic interactions. For this purpose, we utilize the modified Klein-Gordon equation for the Boson particles and then Dirac equations for the fermion particles, respectively. Next, we examine that the Hawking temperature of the black holes do not depend on the properties of tunneling particles. Moreover, we present the corrected Hawking temperature of scalar and fermion particles looks similar in both interactions, but there are different mass and momentum relationships for scalar and fermion particles in cubic and quartic interactions.

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“…Quantum corrections to the thermodynamical quantities for a Bardeen charged regular BH were investigated in [13] using the quantum tunneling approach over semiclassical approximations. In a recent work [14], the effects of noncommutativity on the thermodynamics of this BH were discussed.…”

Section: Introductionmentioning

confidence: 99%

Black hole evaporation in a noncommutative charged Vaidya model

Sharif

Javed

2012

J. Exp. Theor. Phys.

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We study the black hole evaporation and Hawking radiation for a noncommutative charged Vaidya black hole. For this purpose, we determine a spherically symmetric charged Vaidya model and then formulate a noncommutative Reissner-Nordström like solution of this model, which leads to an exact (t -r) depen dent metric. The behavior of the temporal component of this metric and the corresponding Hawking tem perature are investigated. The results are shown in the form of graphs. Further, we examine the tunneling pro cess of charged massive particles through the quantum horizon. We find that the tunneling amplitude is mod ified due to noncommutativity. Also, it turns out that the black hole evaporates completely in the limits of large time and horizon radius. The effect of charge is to reduce the temperature from a maximum value to zero. We note that the final stage of black hole evaporation is a naked singularity.

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Quantum Corrections for a Bardeen Regular Black Hole

Cited by 49 publications

References 20 publications

Quasinormal modes of gravitational perturbation around regular Bardeen black hole surrounded by quintessence

Quasinormal modes of gravitational perturbation around regular Bardeen black hole surrounded by quintessence

Hawking radiation from cubic and quartic black holes via tunneling of GUP corrected scalar and fermion particles

Black hole evaporation in a noncommutative charged Vaidya model

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