Analytical correspondence between shadow radius and black hole quasinormal frequencies

Cuadros-Melgar, Bertha; Fontana, R. D. B.; Oliveira, Jéferson de

doi:10.1016/j.physletb.2020.135966

Cited by 74 publications

(55 citation statements)

References 23 publications

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“…This work is helpful to detect indirectly the dark matter near the event horizon. Subsequently, this correspondence was verified by the 3rd order WKB approximation approach in [54,55] and by the 13th order WKB approximation approach in [56], respectively.…”

Section: (): V-volmentioning

confidence: 66%

The correspondence between shadow and test field in a four-dimensional charged Einstein–Gauss–Bonnet black hole

et al. 2021

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In this paper, we investigate the photon sphere, shadow radius and quasinormal modes of a four-dimensional charged Einstein–Gauss–Bonnet black hole. The perturbation of a massless scalar field in the black hole’s background is adopted. The quasinormal modes are gotten by the 6th order WKB approximation approach and shadow radius, respectively. When the value of the Gauss–Bonnet coupling constant increase, the values of the real parts of the quasinormal modes increase and those of the imaginary parts decrease. The coincidence degrees of quasinormal modes derived by the two approaches increases with the increase of the values of the Gauss–Bonnet coupling constant and multipole number. It shows the correspondence between the shadow and test field in the four-dimensional Einstein–Gauss–Bonnet–Maxwell gravity. The radii of the photon sphere and shadow increase with the decrease of the Gauss–Bonnet coupling constant.

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Section: (): V-volmentioning

confidence: 66%

The correspondence between shadow and test field in a four-dimensional charged Einstein–Gauss–Bonnet black hole

et al. 2021

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“…where l is the multipole number, c is the angular velocity at the unstable null geodesic, and λ denotes the Lyapunov exponent. In recent works, it was argued that the real part of QNMs frequencies and shadow radius (if we also include a sub-leading regime to half of its value) are related as follows (see for details [66,74])…”

Section: Correspondence Between the Shadow Radius And Qnms In Dark Mamentioning

confidence: 99%

Imprints of dark matter on black hole shadows using spherical accretions

Saurabh

Jusufi

2021

Eur. Phys. J. C

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We study the possibility of identifying dark matter in the galactic center from the physical properties of the electromagnetic radiation emitted from an optically-thin disk region around a static and spherically symmetric black hole. In particular, we consider two specific models for the optical-thin disk region: a gas at rest and a gas in a radial free fall. Due to the effect of dark matter on the spacetime geometry, we find that the dark matter can increase or decrease the intensity of the electromagnetic flux radiation depending on the dark matter model. To this end, we analyze two simple dark matter models having different mass functions $${\mathcal {M}}(r)$$ M ( r ) , with a matter mass M, thickness $$\Delta r_s$$ Δ r s along with a dark matter core radius surrounding the black hole. In addition to that, we explore the scenario of a perfect fluid dark matter surrounding the black hole. We show that in order to have significant effect of dark matter on the intensity of the electromagnetic flux radiation, a high energy density of dark matter near the black hole is needed. We also find that the surrounding dark matter distribution plays a key role on the shadow radius and the intensity of the electromagnetic flux radiation, respectively. Finally we have used the relation between the shadow radius and the quasinormal modes (QNMs) to compute the real part of QNM frequencies.

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“…represents the shadow radius of black holes and equals the inverse of the angular velocity c in the eikonal limit. Subsequently, this relation was improved [51] for a highdimensional static spherically symmetric black hole in terms of the WKB method, i.e., Re ω l 1 = l+ D−3 2 R sh . Therefore, the improved expression of the quasinormal mode frequencies in the eikonal limit for a high-dimensional static spherically symmetric black hole takes the form,…”

Section: Quasinormal Mode Frequencies In the Eikonal Limit Calculatedmentioning

confidence: 99%

High-dimensional Schwarzschild black holes in scalar–tensor–vector gravity theory

Cai

Miao

2021

Eur. Phys. J. C

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We obtain a high-dimensional Schwarzschild black hole solution in the scalar–tensor–vector gravity (STVG), and then analyze the influence of parameter $$\alpha $$ α associated with a deviation of the STVG theory from General Relativity on event horizons and Hawking temperature. We calculate the quasinormal mode frequencies of massless scalar field perturbations for the high-dimensional Schwarzschild STVG black hole by using the sixth-order WKB approximation method and the unstable null geodesic method in the eikonal limit. The results show that the increase of parameter $$\alpha $$ α makes the scalar waves decay slowly, while the increase of the spacetime dimension makes the scalar waves decay fast. In addition, we study the influence of parameter $$\alpha $$ α on the shadow radius of this high-dimensional Schwarzschild STVG black hole and find that the increase of parameter $$\alpha $$ α makes the black hole shadow radius increase, but the increase of the spacetime dimension makes the black hole shadow radius decrease. Finally, we investigate the energy emission rate of the high-dimensional Schwarzschild STVG black hole, and find that the increase of parameter $$\alpha $$ α makes the evaporation process slow, while the increase of the spacetime dimension makes the process fast.

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Analytical correspondence between shadow radius and black hole quasinormal frequencies

Cited by 74 publications

References 23 publications

The correspondence between shadow and test field in a four-dimensional charged Einstein–Gauss–Bonnet black hole

The correspondence between shadow and test field in a four-dimensional charged Einstein–Gauss–Bonnet black hole

Imprints of dark matter on black hole shadows using spherical accretions

High-dimensional Schwarzschild black holes in scalar–tensor–vector gravity theory

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