Motion of particles and gravitational lensing around the (2+1)-dimensional BTZ black hole in Gauss–Bonnet gravity

Narzilloev, Bakhtiyor; Shaymatov, Sanjar; Hussain, Ibrar; Abdujabbarov, Ahmadjon; Ahmedov, Bobomurat; Bambi, Cosimo

doi:10.1140/epjc/s10052-021-09617-4

Cited by 32 publications

(7 citation statements)

References 111 publications

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“…Gravitational lensing was first studied in the weak-field limit, and afterward, these studies were extended to the strong-field limit [14][15][16][17]. To analyze different spacetime parameters in BH spacetimes, gravitational lensing has been investigated by various studies [9,[18][19][20][21]. Bozza et.…”

Section: Introductionmentioning

confidence: 99%

Weak deflection angle and shadow cast by the charged-Kiselev black hole with cloud of strings in plasma*

Atamurotov

Hussain²,

Mustafa³

et al. 2023

Chinese Phys. C

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In this work, the gravitational deflection angle of photon in the weak field limit (or the weak deflection angle) and shadow cast by the electrically charged and spherically symmetric static Kiselev black hole (BH) in the string cloud background are investigated. The influence of the BH charge $Q$, the quintessential parameter $\gamma$ and the string cloud parameter $a$ is studied on the weak deflection angle using the Gauss-Bonnet theorem, on the radius of photon spheres and on the size of the BH shadow in the spacetime geometry of the charged-Kiselev BH in string clouds. Moreover, we study the effects of plasma (uniform and non-uniform) on the weak deflection angle and on the shadow cast by the charged-Kiselev BH surrounded by the clouds of strings. In the presence of uniform/nonuniform plasma medium, increase in the cloud of string parameter $a$, increases the deflection angle $\alpha$. On the other hand decrease in the BH charge $Q$, decreases the deflection angle. Further we observe that an increase of the BH charge $Q$ causes a decrease in the size of the shadow of the BH. We notice that with increase in the values of the parameters $\gamma$ and $a$, the size of the BH shadow also increases and therefore the intensity of the gravitational field around the charged-Kiselev BH in string clouds increases. Thus the gravitational field of the charged-Kiselev BH in string cloud background would be stronger than the field produced by the pure Reissner-Nordstrom BH. Moreover, we use the data released by the Event Horizon Telescope (EHT) collaboration, for the supermassive BHs M87* and Sgr A*, to obtain constraints on the values of the parameters $\gamma$ and $a$.

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Section: Introductionmentioning

confidence: 99%

Weak deflection angle and shadow cast by the charged-Kiselev black hole with cloud of strings in plasma*

Atamurotov

Hussain²,

Mustafa³

et al. 2023

Chinese Phys. C

Self Cite

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“…The strong gravitational lensing was proposed and considered by Virbhadra and Ellis [37]. Following that, an extensive body of work has been done in a wide variety of contexts [see, for example, [38][39][40][41][42][43][44][45][46][47][48][49][50]]. From an astrophysical point of view, all photons mostly go through a plasma medium.…”

Section: Introductionmentioning

confidence: 99%

Shadows and gravitational weak lensing by the Schwarzschild black hole in the string cloud background with quintessential field*

et al. 2022

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In this work, we observe that in the presence of the string cloud parameter $a$ and the quintessence parameter $\gamma$, with the equation of state parameter $\omega_q={-2}/{3}$ the radius of the shadow of the Schwarzschild black hole increases as compared with the pure Schwarzschild black hole case. The existence of both quintessential dark energy and cloud of strings magnify the shadow size and hence the strength of the gravitational field around the Schwarzschild black hole increases. Using the data collected by the Event Horizon Telescope (EHT) collaboration for the M87* and Sgr A*, we obtain upper bounds on the values of the parameters $a$ and $\gamma$. Further, we see the effects of the parameters $a$ and $\gamma$ on the rate of emission energy for the Schwarzschild black hole. We notice that the rate of emission energy is higher in the presence of clouds of string and quintessence. Moreover, we study the weak deflection angle using the Gauss-Bonnet theorem. We show the influence of the cloud of string parameter $a$ and the quintessential parameter $\gamma$ on the weak deflection angle. We notice that both the parameters $a$ and $\gamma$ increase the deflection angle $\alpha$.

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“…Until recently, the Event Horizon Telescope collaboration unveiled the first image of the shadow of a black hole in the electromagnetic regime [2][3][4], which again confirmed the correctness of Einstein's General Theory of Relativity [5] as a model for compact objects with an extreme gravitational field. With the only confirmation of black hole's physical existence, one can not underestimate the progress of theoretical research on the search for the most realistic model of a black hole, as well as its dynamical interactions to any astrophysical environments [6][7][8][9][10][11][12][13][14][15][16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Dark matter effect on the weak deflection angle by black holes at the center of Milky Way and M87 galaxies

Pantig,

Övgün

2022

Preprint

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In this paper, we investigated the effect of dark matter on the weak deflection angle by black holes at the galactic center. We consider three known dark matter density profiles such as the Cold Dark Matter (CDM), Scalar Field Dark Matter (SFDM), and the Universal Rotation Curve (URC) from the Burkert profile. To achieve this goal, we used how the positional angles are measured by Ishihara et al. method based on Gauss-Bonnet theorem (GBT) on the optical metric. With the help of the non-asymptotic form of the GBT, the longitudinal angle difference is also calculated. First, we find the emergence of apparent divergent terms on the said profiles, which indicates that the spacetime describing the black hole-dark matter combination is non-asymptotic. We showed that these apparent divergent terms vanish when the distance of the source and receiver are astronomically distant from the black hole. Using the current observational data in the Milky Way and M87 galaxies, we find interesting behaviors of how the weak deflection angle varies with the impact parameter, which gives us some hint on how dark matter interacts with the null particles for each dark matter density profile. We conclude that since these deviations are evident near the dark matter core radius, the weak deflection angle offers a better alternative for dark matter detection than using the deviation from the black hole shadow. With the DM profiles explored in this study, we find that SFDM is the most difficult to detect, while the easiest is the URC profile.

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Motion of particles and gravitational lensing around the (2+1)-dimensional BTZ black hole in Gauss–Bonnet gravity

Cited by 32 publications

References 111 publications

Weak deflection angle and shadow cast by the charged-Kiselev black hole with cloud of strings in plasma*

Weak deflection angle and shadow cast by the charged-Kiselev black hole with cloud of strings in plasma*

Shadows and gravitational weak lensing by the Schwarzschild black hole in the string cloud background with quintessential field*

Dark matter effect on the weak deflection angle by black holes at the center of Milky Way and M87 galaxies

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