Greybody factor for black string in dRGT massive gravity

Boonserm, Petarpa; Ngampitipan, Tritos; Wongjun, Pitayuth

doi:10.1140/epjc/s10052-019-6827-z

Cited by 51 publications

(32 citation statements)

References 104 publications

(125 reference statements)

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“…Clearly, when m g is taken to be zero, the solution reduces to the usual Schwarzschild geometry of General Relativity. The corresponding metric A(r) has been obtained, for instance, in [15,48]. It is important to mention that the strong coupling scale of the dRGT massive gravity theory was estimated in [48].…”

Section: Field Equations and Vacuum Solution In Massive Gravitymentioning

confidence: 99%

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ISCOs and OSCOs in the Presence of a Positive Cosmological Constant in Massive Gravity

et al. 2021

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We study the impact of a non-vanishing (positive) cosmological constant on the innermost and outermost stable circular orbits (ISCOs and OSCOs, respectively) within massive gravity in four dimensions. The gravitational field generated by a point-like object within this theory is known, generalizing the usual Schwarzschild–de Sitter geometry of General Relativity. In the non-relativistic limit, the gravitational potential differs by the one corresponding to the Schwarzschild–de Sitter geometry by a term that is linear in the radial coordinate with some prefactor γ, which is the only free parameter. Starting from the geodesic equations for massive test particles and the corresponding effective potential, we obtain a polynomial of fifth order that allows us to compute the innermost and outermost stable circular orbits. Next, we numerically compute the real and positive roots of the polynomial for several different structures (from the hydrogen atom to stars and globular clusters to galaxies and galaxy clusters) considering three distinct values of the parameter γ, determined using physical considerations, such as galaxy rotation curves and orbital precession. Similarly to the Kottler spacetime, both ISCOs and OSCOs appear. Their astrophysical relevance as well as the comparison with the Kottler spacetime are briefly discussed.

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Section: Field Equations and Vacuum Solution In Massive Gravitymentioning

confidence: 99%

“…The corresponding metric A(r) has been obtained, for instance, in [15,48]. It is important to mention that the strong coupling scale of the dRGT massive gravity theory was estimated in [48].…”

Section: Field Equations and Vacuum Solution In Massive Gravitymentioning

confidence: 99%

ISCOs and OSCOs in the Presence of a Positive Cosmological Constant in Massive Gravity

et al. 2021

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“…If the gravitational potential is high enough, then we use the WKB approximation method to derived the greybody factor [78]. Another attractive ways to calculate the bound of greybody factor are [79]- [87]. The basis purpose of this paper is to deeply analyze how a deflection angle effect on the plasma and non-plasma medium of a magnetized regular black hole (MRBH).…”

Section: Introductionmentioning

confidence: 99%

Weak Deflection Angle and Greybody Bound of Magnetized Regular Black Hole

Javed¹,

Riaz²,

Овгун³

2022

Preprint

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In this paper, we examine the weak deflection angle and greybody factor of magnetized regular black hole. We implement the Gauss-Bonnet theorem on magnetized regular black hole to get the deflection angle. Moreover, we analyze the influence of plasma and non-plasma mediums on deflection angle of magnetized regular black hole. We observe the graphical behaviour of plasma and non-plasma mediums on deflection angle of magnetized regular black hole. Lastly, we study the rigorous bound phenomenon of the greybody factor of magnetized regular black hole. For this purpose we calculate greybody factor results and analyze the graphical behaviour of greybody bound for the different values of the parameters.

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“…Namely, Hawking radiation which is modified from the perfect black body spectrum is known as the GF [32,33]. There are different methods to compute the GF such as the WKB approximation [34,35], matching method [36,37], rigorous bound method [38], and analytical method for the various of spin fields [39][40][41][42][43][44]. Furthermore, in the framework of GR for the radiation of gravitational waves, the most important phase described in function of the proper oscillation frequencies of the black hole is called QNMs, which depend on the black hole parameters [46,47].…”

Section: Introductionmentioning

confidence: 99%

Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model

Kanzi

Сакалли

2021

Eur. Phys. J. C

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In the framework of the Lorentz symmetry breaking (LSB), we investigate the quasinormal modes (QNMs) and the greybody factors (GFs) of the Kerr-like black hole spacetime obtained from the bumblebee gravity model. In particular, we analyze the scalar and fermionic perturbations of the black hole within the framework of both semi-analytic WKB method and the time domain approach. The impacts of the LSB on the bosonic/fermionic QNMs and GFs of the Kerr-like black hole are investigated in detail. The obtained results are graphically depicted and discussed.

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Greybody factor for black string in dRGT massive gravity

Cited by 51 publications

References 104 publications

ISCOs and OSCOs in the Presence of a Positive Cosmological Constant in Massive Gravity

ISCOs and OSCOs in the Presence of a Positive Cosmological Constant in Massive Gravity

Weak Deflection Angle and Greybody Bound of Magnetized Regular Black Hole

Greybody radiation and quasinormal modes of Kerr-like black hole in Bumblebee gravity model

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