Marginally stable circular orbits in the Schwarzschild black hole surrounded by quintessence matter

Hussain, Ibrar; Ali, Sajid

doi:10.1140/epjp/i2016-16275-3

Cited by 32 publications

(17 citation statements)

References 42 publications

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“…The universe accelerating expansion demands the state parameter to be in range −1 < ω < −1/3. The recent works generalized this result to Kerr black hole by Janis-Newman algorithm (Ghosh (2016);Toshmatov et al (2015)), and the spacetime metric were studied (Hussain & Ali (2016);Oteev et al (2016); Schee & Stuchlik (2016)). Following these works, we generalize Kerr black hole solutions to Kerr-Newman black hole solutions in quintessential dark energy.…”

Section: Introductionmentioning

confidence: 93%

Kerr-Newman-AdS black hole in quintessential dark energy

Wang

2017

Phys. Rev. D

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Quintessential dark energy with pressure p and density ρ is related by equation of state p = ωρ with the state parameter −1 < ω < −1/3. The cosmological dark energy influence on black hole spacetime are interesting and important. In this paper, we study the Kerr-Newman-AdS solutions of the Einstein-Maxwell equation in quintessence field around a black hole by Newman-Janis algorithm and complex computations. From the horizon structure equation, we obtain the expression between quintessence parameter α and cosmological constant Λ if the black hole exists two cosmological horizon r q and r c when ω = −2/3, the result is different from rotational black hole in quintessence matter situation. Through analysis we find that the black hole charge cannot change the value of α. But the black hole spin and cosmological constant are opposite. The black hole spin and cosmological constant make the maximum value of α to become small. The existence of four horizon leads seven types of extremal black holes to constraint the parameter α. With the state parameter ω ranging from −1 to −1/3, the maximum value of α changes from Λ to 1. When ω → −1, the quintessential dark energy likes cosmological constant. The singularity of the black holes is the same with that of Kerr black hole. We also discuss the rotation velocity of the black holes on the equatorial plane for ω = −2/3, −1/2 and −1/3. For small value of α, the rotation velocity on the equatorial plane is asymptotically flat and it can explain the rotation curves in spiral galaxies.

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Section: Introductionmentioning

confidence: 93%

Kerr-Newman-AdS black hole in quintessential dark energy

Wang

2017

Phys. Rev. D

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“…The thin disk is assumed to have an inner edge defined by the marginally stable circular radius r ms , while the orbits at higher radii than r = r ms are Keplerian. Note that marginally stable circular orbits play a crucial role when an accreting BH is surrounded, e.g., by quintessence matter [16,62]. The generic Eqs.…”

Section: Generic Rotating Spacetimementioning

confidence: 99%

Accretion disk around the rotating Damour–Solodukhin wormhole

Karimov¹,

Izmailov²,

Nandi³

2019

Eur. Phys. J. C

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A new rotating generalization of the Damour-Solodukhin wormhole (RDSWH), called Kerr-like wormhole, has recently been proposed and investigated by Bueno et al. for echoes in the gravitational wave signal. We show a novel feature of the RDSWH, viz., that the kinematic properties such as the ISCO or marginally stable radius r ms , efficiency and the disk potential V eff are independent of λ (which means they are identical to their KBH counterparts for any given spin). Differences however appear in the emissivity properties for higher values 0.1 < λ ≤ 1 (say) and for the extreme spin a = 0.998. The kinematic and emissivity are generic properties as variations of the wormhole mass and the rate of accretion within the model preserve these properties. Specifically, the behavior of the luminosity peak is quite opposite to each other for the two objects, which could be useful from the viewpoint of observations. Apart from this, an estimate of the difference Δ λ in the maxima of flux of radiation F(r) shows non-zero values but is too tiny to be observable at present for λ < 10 −3 permitted by the strong lensing bound. The broad conclusion is that RDSWH are experimentally indistinguishable from KBH by accretion characteristics.

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“…The radial null and timelike geodesics describe the formation jets in black hole spacetimes where the particle moves radially. A vast literature exist on the timelike and null particle motion in black hole spacetimes [4][5][6][7][8][9][10][11][12][13]. Different authors have been considered charged and neutral particle motion in the vicinity of different static and rotating black holes with and without charge [14][15][16][17][18][19].…”

Section: Introductionmentioning

confidence: 99%

“…Further, it is observed there, with the increase in the value of the string cloud parameter, the particle can more easily escape to infinity. In another recent work, the effect of the quintessence, which is an appealing candidate for the accelerated expansion of our Universe, has been studied on the motion of particles in the spacetime of the Schwarzschild black hole [12], where it is shown that the quintessence field pushes the circular orbits away from the central object, i.e., the radii of the circular orbits are larger than the radii of the circular orbits in the pure Schwarzschild case. Null particle dynamics in the Schwarzschild black hole with quintessence have been analyzed by Fernando for some particular values of the equation of state parameter [40].…”

Section: Introductionmentioning

confidence: 99%

Radial and circular motion of photons and test particles in the Schwarzschild black hole with quintessence and string clouds

Mustafa

Hussain

2021

Eur. Phys. J. C

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The null and timelike geodesic motion in the vicinity of the Schwarzschild black hole in the presence of the string cloud parameter a and the quintessence field parameter q is studied. The ranges for both the parameters a and q are determined, which allow the existence of the black hole. In the radial motion of photon, the coordinate time t first decreases with the increasing values of both the parameters a and q and then in the close proximity of the horizon of the black hole, there is a turning point, after which the effect of the quintessence field is just opposite on the time t. For the massive particles, the proper time $$\tau $$ τ decreases with increasing values of the parameter a and increases with increase in the value of the parameter q. In the same case of the massive particles, the coordinate time t decreases with increase in the values of both the parameters a and q. Further, it is found that for test particles, the stable circular orbits exist in this spacetime for small values of both the parameters i.e., for $$0<a\ll 1$$ 0 < a ≪ 1 and $$0<q\ll 1$$ 0 < q ≪ 1 . It is observed that the radii of the null circular orbits increase as the values of the parameters a and q increase. While in the case of the timelike geodesics, the radii of the circular orbits increase as the value of the parameter a increases, and they decrease as the value of the parameter q increases.

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Marginally stable circular orbits in the Schwarzschild black hole surrounded by quintessence matter

Cited by 32 publications

References 42 publications

Kerr-Newman-AdS black hole in quintessential dark energy

Kerr-Newman-AdS black hole in quintessential dark energy

Accretion disk around the rotating Damour–Solodukhin wormhole

Radial and circular motion of photons and test particles in the Schwarzschild black hole with quintessence and string clouds

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