Quasi normal modes of hairy black holes at higher-order WKB approach

Avalos, R.; Contreras, Ernesto

doi:10.1140/epjc/s10052-023-11288-2

Cited by 16 publications

(3 citation statements)

References 82 publications

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“…Finally, for recent studies of QNMs in alternative backgrounds see Refs. [78–86] and references therein.…”

Section: Quasinormal Spectramentioning

confidence: 99%

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

Balart,

Panotopoulos,

Rincón

2023

Fortschritte der Physik

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Energy conditions and quasinormal modes (QNMs) for scalar perturbations of regular charged black holes within the framework of General Relativity coupled to non‐linear electrodynamics (NLE) are discussed. The frequencies are computed numerically adopting the WKB method, while in the eikonal limit an analytic expression for the spectra is obtained. The impact of the electric charge, the angular degree, and the overtone number on the spectra is investigated in detail. All frequencies are characterized by a negative imaginary part, and that each type of energy conditions imply a different quasinormal spectrum are found.

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“…Finally, for recent studies of QNMs in alternative backgrounds see Refs. [78–86] and references therein.…”

Section: Quasinormal Spectramentioning

confidence: 99%

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

Balart,

Panotopoulos,

Rincón

2023

Fortschritte der Physik

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“…The spacetime of Horndeski's theory is invested with the hairy black hole [70][71][72][73][74][75]. The simplest case for the hairy black hole in Horndeski's theory has the radially dependent scalar field [72,[76][77][78][79][80] and has been paid much attention in its existence and instability [81], in the nohair theorem [82], in the thermodynamical property [70], in strong gravitational lensing [83,84], in quasi normal modes at higher-order WKB approach [85], and so on. Neutral timelike particles' bound orbits around the hairy black hole in Horndeski's theory [80] are still missing, which will be performed in this paper.…”

Section: Introductionmentioning

confidence: 99%

Precessing and periodic orbits around hairy black holes in Horndeski’s Theory

Lin

Deng

2023

Eur. Phys. J. C

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We investigate the dynamics of neutral timelike particles around a hairy black hole in Horndeski’s theory, which is characterized by a coupling parameter with the dimension of length. With deriving the particles’ relativistic periastron precessions, a preliminary bound on the hairy black hole is obtained by using the result of the S2 star’s precession with GRAVITY. It is tighter than the previous result constrained by the shadow size from EHT observations of M87* by about 3–4 orders of magnitude. We also analyse the particles’ periodic motions around the hole in the strong gravitational field. It clearly shows that small variations in the coupling parameter can make the neutral particles’ motions back and forth from the quasi-periodic orbits to the periodic orbits or no bound orbit. Our present work might provide hints for distinguishing the hairy black hole in Horndeski’s theory from the classical hole by using the particles’ dynamics in the strong gravitational field.

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“…This method has been applied in the context of the Randall-Sundrum braneworld [26,27] and has also been extended to investigate in other gravitational issues, including new black hole solutions, see, e.g., Refs. [25,[28][29][30][31][32][33][34][35][36][37][38][39][40]. In the present work, while employing the GD method, we intend to extend the AdS-Schwarzschild vacuum solution in the presence of a generic gravitational source, which satisfies the weak energy condition.…”

Section: Introductionmentioning

confidence: 99%

Thermodynamics of deformed AdS-Schwarzschild black hole

Khosravipoor,

Farhoudi

2023

Eur. Phys. J. C

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By implementing the gravitational decoupling method, we find the deformed AdS-Schwarzschild black hole solution when there is also an additional gravitational source, which obeys the weak energy condition. We also deliberately choose its energy density to be a certain monotonic function consistent with the constraints. In the method, there is a positive parameter that can adjust the strength of the effects of the geometric deformations on the background geometry, which we refer to as a deformation parameter. The condition of having an event horizon limits the value of the deformation parameter to an upper bound. After deriving various thermodynamic quantities as a function of the event horizon radius, we mostly focus on the effects of the deformation parameter on the horizon structure, the thermodynamics of the solution and the temperature of the Hawking–Page phase transition. The results show that with the increase of the deformation parameter: the minimum horizon radius required for a black hole to have local thermodynamic equilibrium and the minimum temperature below which there is no black hole decrease, and the horizon radius of the phase transition and the temperature of the first-order Hawking–Page phase transition increase. Furthermore, when the deformation parameter vanishes, the obtained thermodynamic behavior of the black hole is consistent with that stated in the literature.

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Quasi normal modes of hairy black holes at higher-order WKB approach

Cited by 16 publications

References 82 publications

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

Regular Charged Black Holes, Energy Conditions, and Quasinormal Modes

Precessing and periodic orbits around hairy black holes in Horndeski’s Theory

Thermodynamics of deformed AdS-Schwarzschild black hole

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