Probing a non-linear electrodynamics black hole with thin accretion disk, shadow, and deflection angle with M87* and Sgr A* from EHT

Uniyal, Akhil; Pantig, Reggie C.; Овгун, Али

doi:10.1016/j.dark.2023.101178

Cited by 77 publications

(25 citation statements)

References 142 publications

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“…Such photon rings are a trademark of a given geometry, thus potentially harbouring a way to make robust tests of the Kerr hypothesis [30][31][32][33]. While EHT observations may be successfully reproduced with a Kerr black hole supplied within General Relativistic Magnetic-Hydrodynamical (GRMHD) simulations of an accretion disk model [34], many works in the literature have sought for modifications to GR canonical black holes via addition of new fields [35][36][37][38][39] and hairy black holes [40,41], horizonless compact objects such as naked singularities [42,43], black bounces [44,45], boson stars [46][47][48][49], rotating [50] and asymmetric wormholes [51,52], as well as modified black holes beyond GR within Gauss-Bonnet [53], asymptotic safety [54], noncommutative geometry [55], Einstein-AEther [56], Horndeski theory [57,58], quadratic gravity [59], or braneworlds [60], to mention a few.…”

Section: Shadow and Photon Ring Observationsmentioning

confidence: 99%

“…We proceed first with the black hole configurations: Sch, RN2, RN1, FC1 and FCt, which are depicted in the set of Figures 6, 7, 8, 9, 10, respectively. On the top panel we depict the (normalized) image for the (from left to right) GLM3 (35), GLM1 (36) and GLM2 (37) emission models, while on the bottom panel we include the observed intensity profiles for the same models. There is nothing surprising in these plots as compared to our initial expectations and what we have in the Schwarzschild case of Fig.…”

Section: Generation Of Imagesmentioning

confidence: 99%

“…Figure 11. The optical appearance of EiBI RN0 configurations (top panel) in the GLM3(35), GLM1(36) and GLM2 (37) emission models, and the associated intensity for each of them (bottom panel), displaying the direct (m = 0) and photon ring (m = 1, 2, 3, 4, 5) emissions, respectively, via a number of peaks M > m.…”

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confidence: 99%

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Shadows and photon rings of regular black holes and geonic horizonless compact objects

Olmo¹,

Rosa²,

Rubiera-García³

et al. 2023

Preprint

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The optical appearance of a body compact enough to posses an unstable bound orbit, when surrounded by an accretion disk, is expected to be dominated by a luminous ring of radiation enclosing a central brightness depression known as the shadow, a picture fully backed up by the recent results of the EHT Collaboration. The characterization of both features -ring and shadowdepends on the interaction between the background geometry and the accretion disk, thus being a fertile playground to test our theories on the nature of compact objects and the gravitational field itself in the strong-field regime. In this work we use both features in order to test a continuous family of solutions interpolating between regular black holes and horizonless compact objects, which arise within the Eddington-inspired Born-Infeld theory of gravity, a viable extension of Einstein's General Relativity (GR). To this end we consider seven distinctive classes of such configurations (five black holes and two traversable wormholes) and study their optical appearances under illumination by a geometrically and optically thin accretion disk, emitting monochromatically with three analytic intensity profiles previously suggested in the literature. We build such images and consider the sub-ring structure created by light rays crossing the disk more than once and existing on top of the main ring of radiation. We discuss in detail the modifications as compared to their GR counterparts, the Lyapunov exponents of nearly unstable orbits, as well as the differences between black hole and traversable wormholes for the three intensity profiles. In addition we consider the properties of the shadow region and link them to the calibrated expectations by the EHT Collaboration. I. INTRODUCTIONA. Multimessenger quantum gravity era

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Section: Shadow and Photon Ring Observationsmentioning

confidence: 99%

Section: Generation Of Imagesmentioning

confidence: 99%

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Shadows and photon rings of regular black holes and geonic horizonless compact objects

Olmo¹,

Rosa²,

Rubiera-García³

et al. 2023

Preprint

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show abstract

“…It would take more years, or even more sophisticated equipment, to probe other theories of gravity using the black hole. Ever since many authors have considered exploring the behavior of the classical shadow silhouette for black holes [15,18] described by either a toy model metric or through an alternative theory of gravity [19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36].…”

Section: Introductionmentioning

confidence: 99%

Testing symmergent gravity through the shadow image and weak field photon deflection by a rotating black hole using the M87$$^$$ and Sgr. $$\hbox {A}^$$ results

Pantig

Овгун²,

Demir

2023

Eur. Phys. J. C

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In this paper, we study rotating black holes in symmergent gravity, and use deviations from the Kerr black hole to constrain the parameters of the symmergent gravity. Symmergent gravity induces the gravitational constant G and quadratic curvature coefficient $$c_{\textrm{O}}$$ c O from the flat spacetime matter loops. In the limit in which all fields are degenerate in mass, the vacuum energy $$V_{\textrm{O}}$$ V O can be wholly expressed in terms of G and $$c_{\textrm{O}}$$ c O . We parametrize deviation from this degenerate limit by a parameter $${\hat{\alpha }}$$ α ^ such that the black hole spacetime is dS for $${\hat{\alpha }} < 1$$ α ^ < 1 and AdS for $${\hat{\alpha }} > 1$$ α ^ > 1 . In constraining the symmergent parameters $$c_{\textrm{O}}$$ c O and $${\hat{\alpha }}$$ α ^ , we utilize the EHT observations on the M87* and Sgr. A* black holes. We investigate first the modifications in the photon sphere and shadow size, and find significant deviations in the photonsphere radius and the shadow radius with respect to the Kerr solution. We also find that the geodesics of time-like particles are more sensitive to symmergent gravity effects than the null geodesics. Finally, we analyze the weak field limit of the deflection angle, where we use the Gauss-Bonnet theorem for taking into account the finite distance of the source and the receiver to the lensing object. Remarkably, the distance of the receiver (or source) from the lensing object greatly influences the deflection angle. Moreover, $$c_{\textrm{O}}$$ c O needs be negative for a consistent solution. In our analysis, the rotating black hole acts as a particle accelerator and possesses the sensitivity to probe the symmergent gravity.

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“…In 2008, Gibbons and Werner found a new way to derive deflection angle of the black holes in weak field limits by using Gauss-bonnet theorem on the optical metric for the Schwarzschild black hole [74], then Werner extended it to stationary black holes using the Kerr-Randers optical geometry [75]. Since then, this method of Gibbons-Werner has been used in various papers to show the weak deflection angle of many black holes or wormholes in the literature [39][40][41][42][43][44][45][46][47][48][76][77][78][79][80][81][82][83][84][85][86][87][88][89][90][91][92].…”

Section: Introductionmentioning

confidence: 99%

4D scale-dependent Schwarzschild-AdS/dS black holes: study of shadow and weak deflection angle and greybody bounding

2023

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We investigate the shadow, deflection angle, and the greybody bounding of a Schwarzschild-AdS/dS black hole in scale-dependent gravity. We used the EHT data to constrain the parameter $$\epsilon$$ ϵ . We have found that within the $$1\sigma$$ 1 σ level of uncertainty, $$\epsilon M_0$$ ϵ M 0 ranges at $$10^{-11} - 10^{-16}$$ 10 - 11 - 10 - 16 orders of magnitude for Sgr. A*, and $$10^{-11} - 10^{-17}$$ 10 - 11 - 10 - 17 for M87*. Using these parameters, we explored how the shadow radius behaves as perceived by a static observer. Using the known parameters for Sgr. A* and M87*, we found different shadow cast behavior near the cosmological horizon even if the same scaling parameters were used. We explored the deflection angle $${\hat{\alpha }}$$ α ^ in the weak field limit for both massive and null particles, in addition to the effect of finite distances using the non-asymptotically flat version of the Gauss-Bonnet theorem. We have found that the $${\hat{\alpha }}$$ α ^ strongly depends on massive particles. Tests on $$\epsilon$$ ϵ ’s effect using Sgr. A* is only along points of low impact parameters. For M87*, only the scaled BH in AdS type can be tested at high impact parameters at the expense of very low value for $${\hat{\alpha }}$$ α ^ . We study the rigorous bound on the greybody factor for scalar field emitted from black holes in the theory and show the bound on the transmission probability. The effects of the scale-dependent gravity on the greybody factors are investigated, and the results indicate that the bound on the greybody factor in this case is less than the bound for the Schwarzschild black hole.

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Probing a non-linear electrodynamics black hole with thin accretion disk, shadow, and deflection angle with M87* and Sgr A* from EHT

Cited by 77 publications

References 142 publications

Shadows and photon rings of regular black holes and geonic horizonless compact objects

Shadows and photon rings of regular black holes and geonic horizonless compact objects

Testing symmergent gravity through the shadow image and weak field photon deflection by a rotating black hole using the M87$$^$$ and Sgr. $$\hbox {A}^$$ results

4D scale-dependent Schwarzschild-AdS/dS black holes: study of shadow and weak deflection angle and greybody bounding

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Probing a non-linear electrodynamics black hole with thin accretion disk, shadow, and deflection angle with M87* and Sgr A* from EHT

Cited by 77 publications

References 142 publications

Shadows and photon rings of regular black holes and geonic horizonless compact objects

Shadows and photon rings of regular black holes and geonic horizonless compact objects

Testing symmergent gravity through the shadow image and weak field photon deflection by a rotating black hole using the M87$$^*$$ and Sgr. $$\hbox {A}^*$$ results

4D scale-dependent Schwarzschild-AdS/dS black holes: study of shadow and weak deflection angle and greybody bounding

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Testing symmergent gravity through the shadow image and weak field photon deflection by a rotating black hole using the M87$$^$$ and Sgr. $$\hbox {A}^$$ results