Geodesics and optical properties of a rotating black hole in Randall–Sundrum brane with a cosmological constant

Khan, Saeed Ullah; Ren, Jing

doi:10.1016/j.cjph.2022.06.017

Cited by 12 publications

(4 citation statements)

References 53 publications

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“…Though, the curve showed maxima and minima only a single time, in contrast to the Kerr dS BH [35]. We have observed that by decreasing spin of BH the orbits become more stable contrast to KNK BH [37], also the stability of orbits increases by increasing intensity of scalar filed. It would be useful to discuss that the nature of the effective potential is also checked for the charge parameter as well as the angular momentum but considering the length of the paper, we have excluded some plots.…”

Section: Final Remarksmentioning

confidence: 64%

“…We have explored the Penrose process for extracting energy from KNAdS BH and studied the negative state of energy as well as the efficiency of the process.The efficiency of the Penrose process is higher with the larger values of a as well as α while, it is low with the increase of Q similar to [37]. The decrease in efficiency of the process with charge parameter is similar to the dyonic KN BH [44].…”

Section: Final Remarksmentioning

confidence: 73%

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Imprints of rastall gravity on particle dynamics

Iftikhar,

Aziz,

Manzoor

et al. 2023

Phys. Scr.

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In this paper, we investigate the trajectories of test particle around the Kerr-Newman anti de-Sitter black hole enclosed by scalar field matter in the context of Rastall gravity. We limit our research to the equatorial plane and analyze the dynamics of both null as well as time-like geodesics. We explore the stable regions with respect to the event horizon, radius of photon orbit and the so called static radius for both null as well as time-like particles. We found that the stable point is always less than the cosmological horizon as well as the static radius. We also discuss the energy extraction as well as negative energy state via Penrose process. The efficiency of the process from Kerr-Newman anti de-Sitter black hole is also examined. We observe that the efficiency of the Penrose process increased with the spin parameter as well the intensity of the scalar field around the BH.

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Section: Final Remarksmentioning

confidence: 64%

Section: Final Remarksmentioning

confidence: 73%

Imprints of rastall gravity on particle dynamics

Iftikhar,

Aziz,

Manzoor

et al. 2023

Phys. Scr.

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“…It was also shown that the shadow size increases with the quintessential dark energy parameter. There is yet another interesting recent work [113], where the shadow of a rotating black hole in Randall-Sundrum brane with a cosmological constant has been studied. In this work it was shown that with the increase in the value of the positive cosmological constant, the radius of the black hole increases.…”

Section: Shadow Of Charged Black Hole Immersed In Pfdmmentioning

confidence: 99%

“…This feature has no analogue in our study as our model does not have a cosmological constant. Also the authors in [113] considered the effect of a tidal charge on the black hole shadow, whereas in our case we have considered the effect of PFDM.…”

Section: Shadow Of Charged Black Hole Immersed In Pfdmmentioning

confidence: 99%

Stability, quasinormal modes in a charged black hole in perfect fluid dark matter

Das,

Chowdhury,

Gangopadhyay

2023

Class. Quantum Grav.

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In this work, we study time-like and null geodesics in a charged black hole background immersed in perfect fluid dark matter (PFDM). Using the condition for circular geodesics, we evaluate the energy and angular momentum in terms of the radius (r 0) of the timelike circular orbits. The existence and finiteness of energy and angular momentum constrain the possible range of PFDM parameter (χ) and r 0. In case of null geodesics, we calculate the radius rp of the unstable circular photon orbits. We then use the Lyapunov exponent to study the stability of the geodesics. Then we analyze the critical exponent useful for determining the possibility of detection of gravitational wave signals. After that, we study the perturbation due to a massless scalar field in such a background and calculate the quasinormal mode (QNM) frequencies and their dependence on χ and black hole charge Q. Also, we compare the obtained QNM frequencies both in the exact case and in the eikonal limit. We also calculate the quality factor of the oscillating system and study its dependence on χ and Q. Finally, we evaluate the black hole shadow radius Rs and graphically observe the effect of χ and Q on it.

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