Null geodesics and shadow of 4$D$ Einstein-Gauss-Bonnet black holes surrounded by quintessence

Heydari-Fard, Malihe; Heydari-Fard, Mohaddese

doi:10.48550/arxiv.2109.02059

Cited by 3 publications

(3 citation statements)

References 57 publications

(64 reference statements)

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“…where we have substituted the effective potential from equation (20) and defined the impact parameter, b…”

Section: Null Geodesicsmentioning

confidence: 99%

On null geodesics and shadow of hairy black holes in Einstein-Maxwell-dilaton gravity

Heydari-Fard,

Sepangi

2021

Preprint

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The time-like and null-like geodesics around compact objects are some of the best tools to classify and understand the structure of a space-time. In this paper, we study the null geodesics around charged static dilaton black holes in Einstein-Maxwell-dilaton gravity. The physical parameters for non-radial geodesics including the effective potential, effective force, radius of the photon sphere and impact parameter are obtained and effects of the charge parameter and dilaton coupling constant on these quantities are studied. Possible photon motions for different values of the impact parameter are analyzed and unstable circular orbits and unbounded orbits are plotted. These results are compared to that of the Schwarzschild, Reissner-Nordstrom and GMGHS black holes. Also, we study the shadow cast by a dilaton black hole and investigate how the dilaton coupling affects the size of the black hole shadow. Finally, as an application of null geodesics, we calculate the deflection of light and investigate the effects of the model parameters on the bending angle.

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“…where we have substituted the effective potential from equation (20) and defined the impact parameter, b…”

Section: Null Geodesicsmentioning

confidence: 99%

On null geodesics and shadow of hairy black holes in Einstein-Maxwell-dilaton gravity

Heydari-Fard,

Sepangi

2021

Preprint

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“…Apart from the cosmological constant, Λ [28][29][30], other prescriptions of dark energy consist of different dynamic models. Among others, quintessence [31][32][33][34][35][36][37][38][39][40] provides a dynamical description of dark energy in terms of a minimally coupled scalar field. Regarding the equation of state, , the model's state parameter, ω, usually falls within the range of .…”

Section: Introductionmentioning

confidence: 99%

Shadows of magnetically charged rotating black holes surrounded by quintessence *

et al. 2022

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In this work, we study the optical properties of a class of magnetically charged rotating black hole spacetimes. The black holes in question are assumed to be immersed in the quintessence field, and subsequently, the resulting black hole shadows are expected to be modified by the presence of the dark energy. We investigate the photon region and the black hole shadow, and in particular, their dependence on the relevant physical conditions such as the state parameter of the quintessence, the angular momentum, and the magnitude of the magnetic charge. It is shown that the photon regions sensitively depend on the horizon structure and possess intricate features. Moreover, from the viewpoint of a static observer, we explore a few observables, especially those associated with the distortion of the observed black hole shadows.

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“…The effect of an accelerated expanding universe on the shadow of a black hole is studied in [50]. It is also natural to study the effect of the quintessence dark energy [40,51], and the investigation can bring new insights and impose restrictions on the quintessence model [52]. Shadows affected by other dark energy models are studied in [53,54].…”

Section: Introductionmentioning

confidence: 99%

Shadow and Photon Sphere of Black Hole in Clouds of Strings and Quintessence

He,

Tao,

Xue

et al. 2021

Preprint

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In this work, we study the shadow and photon sphere of the black bole in clouds of strings and quintessence with static and infalling spherical accretions. We obtain the geodesics of the photons near a black hole with different impact parameters b. The string clouds model and quintessence influence the specific intensity by affecting the geodesic and the average radial position of photons.And the range of string clouds parameter a is constrained to ensure that the shadow can be observed. Moreover, we use a model of the photon emissivity j(ν e ) to get the specific intensities.The light sources in the accretion follow a normal distribution with an attenuation factor γ. The shadow with static spherical accretion is plotted. The apparent shape of the shadow is a perfect circle, and the value of γ affects the brightness of the photon sphere. We investigate the profile and specific intensity of the shadows with static and infalling spherical accretions respectively. The interior of the shadows with an infalling spherical accretion will be darker than that with the static spherical accretion, and the specific intensity with both static and infalling spherical accretion gradually converges.

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Null geodesics and shadow of 4$D$ Einstein-Gauss-Bonnet black holes surrounded by quintessence

Cited by 3 publications

References 57 publications

On null geodesics and shadow of hairy black holes in Einstein-Maxwell-dilaton gravity

On null geodesics and shadow of hairy black holes in Einstein-Maxwell-dilaton gravity

Shadows of magnetically charged rotating black holes surrounded by quintessence *

Shadow and Photon Sphere of Black Hole in Clouds of Strings and Quintessence

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