Scalar perturbations and quasi-normal modes of a nonlinear magnetic-charged black hole surrounded by quintessence

Chakrabarty, Hrishikesh; Abdujabbarov, Ahmadjon; Bambi, Cosimo

doi:10.1140/epjc/s10052-019-6687-6

Cited by 26 publications

(14 citation statements)

References 101 publications

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“…An increase in Q leads to the reduction of absorption probability (Figure 3) which is also consistent with the literature [32]. It is found that the greybody factor gets suppressed for larger values of α in comparison with [21] whereas the higher modes of rotation parameter show a substantial increase in the emission rate of massless scalar particles. For the orbital angular momentum, partial wave with smaller values reduce the greybody factor as for the rotating BH [33].…”

Section: Discussionsupporting

confidence: 89%

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Greybody factor for quintessential Kerr–Newman black hole

Sharif

Ama-Tul-Mughani

2020

Physics of the Dark Universe

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In this paper, we formulate an analytic expression of the greybody factor for the Kerr-Newman black hole in the presence of the quintessential field. Primarily, we analyze the profile of effective potential by transforming the radial equation of motion into standard Schrödinger form through tortoise coordinate. The two asymptotic solutions, in the form of hypergeometric functions, are computed at distinct radial regions such as a black hole and cosmological horizons determined by the quintessence. To extend the viability over the whole radial regime, we match the analytical solutions smoothly in an intermediate region by using a semi-classical approach. We also calculate the emission rates and absorption cross-section for the massless scalar fields to elaborate on the significance of our result. It is found that the electromagnetic force together with the gravitational pull of black hole maximizes the effective potential and consequently, decreases the emission process of scalar field particles.

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Section: Discussionsupporting

confidence: 89%

“…Saleh et al [20] studied the quasinormal modes as well as Hawking radiation for quintessential RN BH. Chakrabarty et al [21] analyzed the quasinormal modes as well as greybody factor for the emission of scalar particles around a nonlinear magnetic-charged BH surrounded by quintessence.…”

Section: Introductionmentioning

confidence: 99%

Greybody factor for quintessential Kerr–Newman black hole

Sharif

Ama-Tul-Mughani

2020

Physics of the Dark Universe

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“…In Table I, we provide the ISCO radius obtained by solving Eqs. (19) and (22) numerically for different values of perfect fluid dark matter parameter α and magnetic charge parameter λ in the case of fixed black hole magnetic charge parameter g. The behavior of the results tabulated in Table I is also reflected in Fig. 11.…”

Section: Magnetically Charged Particle Motion Around Bardeen Blamentioning

confidence: 84%

“…Particularly, Kiselev has obtained a black hole solution surrounded by quintessence [18] and its rotational analogue obtained in [19]. The properties of black holes surrounded by quintessence have been studied in [20][21][22][23]. Authors of Refs.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of test particles around a Bardeen black hole surrounded by perfect fluid dark matter

et al. 2020

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We study the dynamics of (i) neutral test particles, (ii) magnetically charged test particles, and (iii) test magnetic dipole around a regular Bardeen black hole surrounded by perfect fluid dark matter (PFDM). It has been shown how the magnetic charge of the black hole and the parameter of the surrounding PFDM can influence the innermost stable circular orbit (ISCO) radius of a test particle. We have found that the ISCO radius is strongly affected as a consequence of the combined effect of the magnetic charge parameter and the perfect fluid dark matter. The black hole magnetic charge parameter g and the combined effect of perfect fluid dark matter can mimic the black hole rotation parameter up to a/M ≈ 0.9. It has been observed that the ISCO for magnetic dipole disappears at the values exceeding the calculated upper value for the magnetic interaction parameter β. The upper limit decreases with the increase of both the dark matter and magnetic charge parameters. Finally, as an astrophysical application, we have analyzed degeneracy effects of spin of Kerr black holes and magnetic charge of regular Bardeen black holes for the different values of the dark matter parameter providing exactly the same value for ISCO radius of a magnetic dipole with the same value of the parameter β = 10.2 of the magnetar called PSR J1745-2900 orbiting around supermassive black hole Sagittarius A*. It has been observed that the magnetic charge of the pure regular Bardeen black hole can mimic the spin of a Kerr black hole up to a/M 0.8085, while upper limit for the magnetic charge which may provide ISCO for the magnetic dipole is gupper 0.65M . In the presence of PFDM with the parameter α = 0.01(0.05), the upper limit for the magnetic charge decreases and equals to gupper 0.62M (0.548M ) and consequently mimicker value for the spin parameter of black hole lies in the range of a/M ∈ (0.0106 ÷ 0.8231) ( a/M ∈ (0.0816 ÷ 0.8595)). We also show that the same values of the spin of Kerr black hole and the magnetic charge of regular Bardeen black hole surrounded by PFDM provide the same values for the ISCO radius of the chosen magnetar.

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“…Based on the quintessence, some exact black hole solutions were gotten and the thermodynamic properties were discussed [44][45][46][47][48][49][50][51]. In the study of the perturbations of the state parameter, Chakrabarty et al found that the perturbations with high value the parameter are unstable [52]. In axisymmetric black holes, the quintessence-like matter changes the shape of the black hole shadow [53].…”

Section: Introductionmentioning

confidence: 99%

Quasinormal modes and the correspondence with shadow in black holes with a deficit solid angle and quintessence-like matter

Yu¹,

Chen²,

Gao³

2022

Preprint

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In this paper, we investigate the photon sphere, shadow radius and quasinormal modes of a 4-dimensional black hole with a deficit solid angle and quintessence-like matter. We find that the radii of the photon sphere and shadow decrease with the decreases of the deficit solid angle and density of quintessence-like matter. The quasinormal modes are gotten by the sixth order WKB approximation method and shadow radius, respectively. The values of the real part and imaginary parts of the quasinormal modes increase with the decrease of the values of the deficit solid angle and density of quintessence-like matter when the multipole number is fixed. The quasinormal modes gotten by these two methods are in good agreement, especially when the multipole number is large. It shows the correspondence between the quasinormal modes in the eikonal limit and shadow.

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Scalar perturbations and quasi-normal modes of a nonlinear magnetic-charged black hole surrounded by quintessence

Cited by 26 publications

References 101 publications

Greybody factor for quintessential Kerr–Newman black hole

Greybody factor for quintessential Kerr–Newman black hole

Dynamics of test particles around a Bardeen black hole surrounded by perfect fluid dark matter

Quasinormal modes and the correspondence with shadow in black holes with a deficit solid angle and quintessence-like matter

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