Dynamics of the particle around de Sitter–Schwarzschild black hole surrounded by quintessence

Khan, Israr Ali; Khan, Amir; Islam, Saeed

doi:10.1142/s0217751x20501304

Cited by 8 publications

(4 citation statements)

References 27 publications

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“…Such features have been discussed extensively in general relativity and alternative gravity theories (see for example [36][37][38][39]). These may include the presence of a dark matter halo [40,41], or coupling with a quintessential field [42][43][44][45]. The standard thermodynamics of static black holes in quintessence has been studied extensively, for example in [46][47][48][49][50][51][52].…”

Section: The Black Hole Solution In the Dark Backgroundmentioning

confidence: 99%

Carathéodory’s thermodynamics of the Schwarzschild black hole surrounded by quintessence

2023

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In this paper, we apply the Carathéodory’s method of geometrothermodynamics to investigate the behavior of the main thermodynamic parameters associated with a Schwarzschild black hole surrounded by quintessence. The corresponding Pfafﬁan form is constructed by means of the Schwarzschild radius rs, and the quintessential radius rγ, as independent variables. This form is then used to characterize the thermodynamic manifold. The homogeneity of the system allows for the recognition of the empirical temperature and entropy, and thus, connects with the usual laws of thermodynamics. In particular, we show that the Helmholtz and Gibbs free energies lead to the same value for the Schwarzschild black hole, in the case of the vanishing cosmological term.

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Section: The Black Hole Solution In the Dark Backgroundmentioning

confidence: 99%

Carathéodory’s thermodynamics of the Schwarzschild black hole surrounded by quintessence

2023

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“…In the case of our paper, we are in an even more extreme situation since we cannot provide an unambiguous physical interpretation to the parameter β because these analyses rely on the study of the geodesic motion which depends on the metric tensor and not the gravitational theory formulation. To our knowledge, this degeneracy has never been pointed out, despite the geodesic motion in the spacetime (1) has been extensively studied in the literature [25,[64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82][83].…”

Section: Physical Interpretation Of β: Accretion Disk and Shadowmentioning

confidence: 99%

A Critical Assessment of Black Hole Solutions With a Linear Term in Their Redshift Function

Gregoris,

Ong,

Wang

2021

Preprint

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Different theories of gravity can admit the same black hole solution, but the parameters usually have different physical interpretations. In this work we study in depth the linear term βr in the redshift function of black holes, which arises in conformal gravity, de Rham-Gabadadze-Tolley (dRGT) massive gravity, f (R) gravity (as approximate solution) and general relativity. Geometrically we quantify the parameter β in terms of the curvature invariants. Astrophysically we found that β can be expressed in terms of the cosmological constant, the photon orbit radius and the innermost stable circular orbit (ISCO) radius. The metric degeneracy can be broken once black hole thermodynamics is taken into account. Notably, we show that under Hawking evaporation, different physical theories with the same black hole solution (at the level of the metric) can lead to black hole remnants with different values of their physical masses with direct consequences on their viability as dark matter candidates. In particular, the mass of the graviton in massive gravity can be expressed in terms of the cosmological constant and of the formation epoch of the remnant. Furthermore the upper bound of remnant mass can be estimated to be around 0.5 × 10 27 kg.

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“…In regards to Kiselev solutions, their rotating counterpart was later constructed [8][9]. The role played by the effects of quintessence on BHs has received considerable attention [10][11][12][13][14][15][16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Greybody factor and perturbation of a Schwarzschild black hole with string clouds and quintessence

Al-Badawi

2022

Preprint

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In this paper, we investigated the Dirac and Klein-Gordan equations, as well as the greybody factor for a Schwarzschild black hole (SBH) immersed in quintessence and associated with a cloud of strings. Primarily, we study the Dirac equation using a null tetrad in the Newman-Penrose (NP) formalism. Next, we separate the Dirac equation into radial and angular sets. Using the radial equations, we study the profile of effective potential by transforming the radial equation of motion into standard Schrödinger wave equations form through tortoise coordinate. Similarly, we study the Klein-Gordan equation in this spacetime. The Miller-Good transformation method is employed to compute the greybody factor of bosons. To compute the Gerybody factor for fermions, we use the general method of semi-analytical bounds. We also investigate the effect of string clouds and quintessence parameters on Hawking radiation. According to the results, the greybody factor is strongly influenced by the shape of the potential, which is determined by the model parameters. This is consistent with the ideas of quantum mechanics; as the potential rises, it becomes harder for the wave to penetrate.

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Dynamics of the particle around de Sitter–Schwarzschild black hole surrounded by quintessence

Cited by 8 publications

References 27 publications

Carathéodory’s thermodynamics of the Schwarzschild black hole surrounded by quintessence

Carathéodory’s thermodynamics of the Schwarzschild black hole surrounded by quintessence

A Critical Assessment of Black Hole Solutions With a Linear Term in Their Redshift Function

Greybody factor and perturbation of a Schwarzschild black hole with string clouds and quintessence

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