Equatorial and Polar Quasinormal Modes and Quasiperiodic Oscillations of Quantum Deformed Kerr Black Hole

Jusufi, Kimet; Azreg‐Aïnou, Mustapha; Jamil, Mubasher; Wu, Qiang

doi:10.3390/universe8040210

Cited by 10 publications

(5 citation statements)

References 44 publications

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“…Substituting equation ( 36) into equation (34), and repeating the procedure to obtain equation (39), then equation ( 34) reduces to…”

Section: First Order Perturbation Equations For Metric and Electromag...mentioning

confidence: 99%

“…Thus it provides us a powerful tool to distinguish different BHs and theories by detecting QNMs in GWs. Amounts of effort have been devoted on studying QNMs of various BHs in variety of theories in past years [39][40][41][42], see also reviews [43][44][45][46]. Although limited by detection accuracy, data analysis to read off QNMs from the detected GW signals are ongoing and some progresses have been made [47][48][49][50][51][52][53][54].…”

Section: Introductionmentioning

confidence: 99%

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Gravito-electromagnetic perturbations and QNMs of regular black holes

Meng,

Zhang

2023

Class. Quantum Grav.

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In the framework of Einstein's gravity coupled to nonlinear electromagnetic fields, we study gravito-electromagnetic perturbations of magnetic regular black holes. The master equations of perturbations are obtained through Chandrasekhar's formulation, from which it can be seen, different from the electric counterparts, for magnetic black holes gravitational perturbations with odd-parity coupled only to the electromagnetic perturbations with even-parity. We solve the master equations numerically and obtain quasinormal modes (QNMs) for three typical regular black holes. Results show that QNMs of distinct regular black holes differ significantly, and they differ from that of the Reissner-Nordstr¨om black hole as well. Indications of these results on the stability of these regular black holes are discussed in detail.

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“…Substituting equation ( 36) into equation (34), and repeating the procedure to obtain equation (39), then equation ( 34) reduces to…”

Section: First Order Perturbation Equations For Metric and Electromag...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gravito-electromagnetic perturbations and QNMs of regular black holes

Meng,

Zhang

2023

Class. Quantum Grav.

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“…The last equation is nothing but the result which was obtained previously in Ref. [110], where the points r ± ph were determined by solving [58,111]…”

Section: Equatorial and Polar Qnms And Their Relation With Typical Sh...mentioning

confidence: 92%

“…Using the metric functions and after some algebraic manipulation in the Eikonal limit we can use Eq. ( 40) which can be further simplified as follows [111]…”

Section: Equatorial and Polar Qnms And Their Relation With Typical Sh...mentioning

confidence: 99%

Shadow and quasinormal modes of the Kerr–Newman–Kiselev–Letelier black hole

et al. 2022

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We investigate the null geodesics and the shadow cast by the Kerr–Newman–Kiselev–Letelier (KNKL) black hole for the equation of state parameter $$\omega _q=-2/3$$ ω q = - 2 / 3 and for different values of the spacetime parameters, including the quintessence parameter $$\gamma $$ γ , the cloud of string (CS) parameter b, the spin parameter a and the charge Q of the black hole. We notice that for the increasing values of the parameters $$\gamma $$ γ and b the size of the shadow of the KNKL black hole increases and consequently the strength of the gravitational field of the black hole increases. On the other hand with increase in the charge Q of the black hole the size of the shadow of the black hole decreases. Further with the increase in the values of the spin parameter a of the KNKL black hole, we see that the distortion of the shadow of the black hole becomes more prominent. Moreover we use the data released by the Event Horizon Telescope (EHT) collaboration, to restrict the parameters b and $$\gamma $$ γ for the KNKL black hole, using the shadow cast by the KNKL black hole. To this end, we also explore the relation between the typical shadow radius and the equatorial and polar quasinormal mods (QNMs) for the KNKL black hole and extend this correspondence to non-asymptotically flat spacetimes. We also study the emission energy rate from the KNKL black hole for the various spacetime parameters, and observe that it increases for the increasing values of both the parameters $$\gamma $$ γ and b for fixed charge-to-mass and spin-to-mass ratios of the KNKL black hole. Finally, we investigate the effects of plasma on the photon motion, size and shape of the shadow cast by the KNKL black hole. While keeping the spacetime parameters fixed, we notice that with increase in the strength of the plasma medium the size of the shadow of the KNKL black hole decreases and therefore the intensity of the gravitational field of the KNKL black hole decreases in the presence of plasma.

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“…On the other hand, since wormholes can be a candidate for the black hole mimicker, then several astrophysical signatures of wormholes have been proposed to search for their existence in near future, for example, the shadow [56][57][58][59][60][61][62], the gravitational lensing [63][64][65][66][67][68][69], the accretion disk around the wormhole [70][71][72], and the ringdown phase in the emission of gravitational waves [73].…”

Section: Introductionmentioning

confidence: 99%

Non-Abelian wormholes threaded by a Yang-Mills-Higgs field in the BPS limit

Chew

Lim

2020

Phys. Rev. D

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We construct numerically the symmetric non-Abelian wormholes which are supported by a phantom field in the Einstein-Yang-Mills-Higgs theory beyond Bogomol'nyi-Prasad-Sommerfield (BPS) limit where the Higgs self-interaction constant λ is non-vanishing. Analogous to the BPS limit, the probe limit is the Yang-Mills-Higgs field in the background of the Ellis wormhole when the gravity is switched off. In the presence of gravity, the wormhole solutions possess the Yang-Mills-Higgs hair where families of hairy wormholes solutions emerge from the Ellis wormhole when the gravitational coupling constant increases. In contrast to the BPS limit, the properties of wormholes change drastically when the gravitational strength approaches a critical value for a fixed λ. The hairy wormholes possess two types of double throat configurations. The first type is wormholes that develop the double throat when the gravitational strength almost approaches the critical value for lower λ, whereas the second type is wormholes that exhibit the double throat for a certain range of gravitational strength for higher λ. These two types of double throat configurations can coexist for a certain range of λ where it is a transition process for first type double throat disappears gradually and the second type double throat becomes dominant.

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Equatorial and Polar Quasinormal Modes and Quasiperiodic Oscillations of Quantum Deformed Kerr Black Hole

Cited by 10 publications

References 44 publications

Gravito-electromagnetic perturbations and QNMs of regular black holes

Gravito-electromagnetic perturbations and QNMs of regular black holes

Shadow and quasinormal modes of the Kerr–Newman–Kiselev–Letelier black hole

Non-Abelian wormholes threaded by a Yang-Mills-Higgs field in the BPS limit

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