QED effect on a black hole shadow

Hu, Zezhou; Zhong, Zhen; Li, Peng-Cheng; Guo, Minyong; Chen, Bin

doi:10.1103/physrevd.103.044057

Cited by 70 publications

(51 citation statements)

References 94 publications

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“…We did not consider synchrotron self-absorption [5], which is desirable when studying the background emission of the plasma. It would also be interesting to take the black hole spin [28][29][30][31][32][33][34][35] and the QED effect [36] into account.…”

Section: Discussionmentioning

confidence: 99%

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Gravitational effect of plasma particles on the shadow of Schwarzschild black holes

Zhu

Wang

2022

Eur. Phys. J. C

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Considering a Schwarzschild black hole surrounded by a fully ionized hydrogen plasma, we study the effect of the gravitational field of the plasma particles on the shadow. We take a formalism in which this effect is unified with the refractive effect of the plasma medium studied previously, but the two effects are characterized by two independent parameters. For semi-realistic values of parameters, we find their corrections to the shadow radius are both negligible, and the gravitational correction can overtake the refractive correction for active galactic nuclei of masses larger than $$10^9M_{\odot }$$ 10 9 M ⊙ . With unrealistically large values of parameters, we illustrate the two effects on the light trajectories and the intensity map.

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Section: Discussionmentioning

confidence: 99%

“…Corresponding to (36), the event horizon of black hole is located at r = r g , and the cosmological horizon is located at…”

Section: Model B: R C = 3r Gmentioning

confidence: 99%

Gravitational effect of plasma particles on the shadow of Schwarzschild black holes

Zhu

Wang

2022

Eur. Phys. J. C

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“…For the Kerr and Kerr-Newman metric, K (r ) = r 2 , and the above expression reduces to ψ = r 2 +a 2 cos 2 θ . After substituting ψ (39) into the general form of the rotating spacetime metric (37), if the static spacetime metric (10) can be obtained in the limit a → 0, the rotating solution is known as normal fluid; otherwise it is known as conformal fluid. Normal fluid solution requires lim a→0 ψ(r, θ, a) = H (r ) (40) which implies F(r ) = G(r ).…”

Section: Newman-janis Algorithm Without Complexificationmentioning

confidence: 99%

“…Similar shadows can also be cast by other compact objects. There are several literature where the shadows cast by compact objects such as black holes, naked singularities, gravastar and wormholes are extensively studied [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37]. In [38], authors discuss the shadow cast by Joshi-Malafarina-Narayan (JMN) naked singularity spacetime and they compare the results with a shadow cast by the Schwarzschild black hole.…”

Section: Introductionmentioning

confidence: 99%

Shadows and precession of orbits in rotating Janis–Newman–Winicour spacetime

et al. 2022

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In this paper, we construct the rotating Janis–Newman–Winicour (JNW) naked singularity spacetime using Newman–Janis Algorithm (NJA). We analyse NJA with and without complexification methods and find that the energy conditions do satisfied when we skip the complexification step. We study the shadows cast by rotating JNW naked singularity and compare them with the shadows cast by the Kerr black hole. We find that the shadow of the rotating naked singularity can be distinguished from the shadow of the Kerr black hole. While we analyse the precession of timelike bound orbits in rotating JNW spacetime, we find that it can have a negative (or opposite) precession, which is not present in the Kerr black hole case. These novel signatures of the shadow and orbital precession in rotating JNW naked singularity spacetime could be important in the context of the recent observation of the shadow of the M87 galactic center and the stellar dynamics of ‘S-stars’ around Milkyway galactic center.

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Section: Introductionmentioning

confidence: 99%

Shadows and precession of orbits in rotating Janis-Newman-Winicour spacetime

Solanki,

Bambhaniya,

Dey

et al. 2021

Preprint

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In this paper, we construct the rotating Janis-Newman-Winicour (JNW) naked singularity spacetime using Newman-Janis Algorithm (NJA). We analyse NJA with and without complexification methods and find that the energy conditions do satisfied when we skip the complexification step. We study the shadows cast by rotating JNW naked singularity and compare them with the shadows cast by the Kerr black hole. We find that the shadow of the rotating naked singularity can be distinguished from the shadow of the Kerr black hole. While we analyse the precession of timelike bound orbits in rotating JNW spacetime, we find that it can have a negative (or opposite) precession, which is not present in the Kerr black hole case. These novel signatures of the shadow and orbital precession in rotating JNW naked singularity spacetime could be important in the context of the recent observation of the shadow of the M87 galactic center and the stellar dynamics of 'S-stars' around Milkyway galactic center.

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QED effect on a black hole shadow

Cited by 70 publications

References 94 publications

Gravitational effect of plasma particles on the shadow of Schwarzschild black holes

Gravitational effect of plasma particles on the shadow of Schwarzschild black holes

Shadows and precession of orbits in rotating Janis–Newman–Winicour spacetime

Shadows and precession of orbits in rotating Janis-Newman-Winicour spacetime

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