Shadow of five-dimensional rotating Myers-Perry black hole

Papnoi, Uma; Atamurotov, Farruh; Ghosh, Sushant G.; Ahmedov, Bobomurat

doi:10.1103/physrevd.90.024073

Cited by 213 publications

(133 citation statements)

References 63 publications

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“…a dark area in front of a luminous background [56,59]. Hence, their is a significant effort to study black hole shadows and this has become a quite active research field [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48] (for a review, see [60]). For the Schwarzschild black hole the shadow of the black hole is a perfect circle [60], and it is enlarged in the case of a Reissner-Nordström black hole [61].…”

Section: Shadow Of Einstein-born-infeld Black Holementioning

confidence: 99%

“…The photons that cross the event horizon, due to strong gravity, are removed from the observable universe which lead to a shadow (silhouette) imprinted by a black hole on the bright emission that exists in its vicinity. So far the shadows of the compact gravitational objects in the different cases have been extensively studied, see, e.g., [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48]. Furthermore a new general formalism to describe the shadow of black hole as an arbitrary polar curve expressed in terms of a Legendre expansion was developed in a recent paper [49].…”

Section: Introductionmentioning

confidence: 99%

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Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

2016

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We investigate the horizon structure of the rotating Einstein-Born-Infeld solution which goes over to the Einstein-Maxwell's Kerr-Newman solution as the BornInfeld parameter goes to infinity (β → ∞). We find that for a given β, mass M, and charge Q, there exist a critical spinning parameter a E and r E H , which corresponds to an extremal Einstein-Born-Infeld black hole with degenerate horizons, and a E decreases and r E H increases with increase of the Born-Infeld parameter β, while a < a E describes a non-extremal Einstein-Born-Infeld black hole with outer and inner horizons. Similarly, the effect of β on the infinite redshift surface and in turn on the ergo-region is also included. It is well known that a black hole can cast a shadow as an optical appearance due to its strong gravitational field. We also investigate the shadow cast by the both static and rotating Einstein-Born-Infeld black hole and demonstrate that the null geodesic equations can be integrated, which allows us to investigate the shadow cast by a black hole which is found to be a dark zone covered by a circle. Interestingly, the shadow of an Einstein-Born-Infeld black hole is slightly smaller than for the Reissner-Nordstrom black hole, which consists of concentric circles, for different values of the Born-Infeld parameter β, whose radius decreases with increase of the value of the parameter β. Finally, we have studied observable distortion parameter for shadow of the rotating Einstein-Born-Infeld black hole. a e-mails: farruh@astrin.uz;

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Section: Shadow Of Einstein-born-infeld Black Holementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

2016

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“…The issue of the separability of the Hamilton-Jacobi equation in higher dimensional space-time has been widely studied in the literature [32][33][34]. Particularly, the authors of Refs.…”

Section: Geodesics and Circular Orbitsmentioning

confidence: 99%

Energetics and optical properties of 6-dimensional rotating black hole in pure Gauss–Bonnet gravity

Abdujabbarov¹,

et al. 2015

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We study physical processes around a rotating black hole in pure Gauss-Bonnet (GB) gravity. In pure GB gravity, the gravitational potential has a slower fall-off as compared to the corresponding Einstein potential in the same dimension. It is therefore expected that the energetics of a pure GB black hole would be weaker, and our analysis bears out that the efficiency of energy extraction by the Penroseprocess is increased to 25.8 % and the particle acceleration is increased to 55.28 %; the optical shadow of the black hole is decreased. These are in principle distinguishing observable features of a pure GB black hole.

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“…Select approaches include analyzing the shadow characteristics of Kerr black holes with scalar hair [11], a five-dimensional Myers-Perry black hole [12], distorted Schwarzschild [13] and Kerr black holes [14], as well as the possibility of observing double images from a single black hole [15]. Additional shadow traits in other extensions and alternatives to general relativity include noncommutative gravity inspired black holes [16], Modified Gravity [17], f (r) gravity [18], a rotating Einstein-Born-Infeld black hole [19], regular black holes [20], and rotating non-singular black holes [21].…”

Section: Introductionmentioning

confidence: 99%

Black hole shadows in fourth-order conformal Weyl gravity

Mureika

Varieschi

2017

Can. J. Phys.

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We calculate the characteristics of the "black hole shadow" for a rotating, neutral black hole in fourth-order conformal Weyl gravity. It is shown that the morphology is not significantly affected by the underlying framework, except for very large masses. Conformal gravity black hole shadows would also significantly differ from their general relativistic counterparts if the values of the main conformal gravity parameters, γ and κ, were increased by several orders of magnitude. Such increased values for γ and κ are currently ruled out by gravitational phenomenology. Therefore, it is unlikely that these differences in black hole shadows will be detected in future observations, carried out by the Event Horizon Telescope or other such experiments.

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Shadow of five-dimensional rotating Myers-Perry black hole

Cited by 213 publications

References 63 publications

Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

Horizon structure of rotating Einstein–Born–Infeld black holes and shadow

Energetics and optical properties of 6-dimensional rotating black hole in pure Gauss–Bonnet gravity

Black hole shadows in fourth-order conformal Weyl gravity

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