Optical appearance of Einstein-Æther black hole surrounded by thin disk

Wang, Huimin; Lin, Zi-Chao; Wei, Shao-Wen

doi:10.48550/arxiv.2205.13174

Cited by 2 publications

(3 citation statements)

References 79 publications

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“…Faraji et al in their recent paper confirmed that the quadrupole parameter plays a non-negligible role in the physical properties of the thin disk solution around twisted Schwarzschild spacetime [54]. Recently, efforts have been devoted to studying the shadows and the observational appearance of black holes which are surrounded by spherically symmetric accretion and thin disk accretion [21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36]. Considering both the static and infalling spherically symmetric accretion models, the inner region of the infalling one is darker than that of the static one due to the Doppler effect [23,24].…”

Section: Introductionmentioning

confidence: 98%

“…Considering both the static and infalling spherically symmetric accretion models, the inner region of the infalling one is darker than that of the static one due to the Doppler effect [23,24]. Also, under the background that black holes are surrounded by the thin disk accretion, the light rays around black holes can be divided into three types, i.e., direct emission, lens ring and photon ring [23,24,27,30,[32][33][34][35][36]. Moreover, there are differences in the contributions of direct emission, lens rings and photon rings to the observed intensity of black holes.…”

Section: Introductionmentioning

confidence: 99%

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Shadows and observational appearance of a new family of Ayón-Beato-García black holes

Mou¹,

Chen²,

He³

et al. 2022

Commun. Theor. Phys.

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In this paper, we study the shadows and observational appearance of the Ayón-Beato-García (ABG) black hole, which is surrounded by a thin disk accretion. For a four-dimensional ABG black hole, as the charge q increases, the event horizon $r_+$, radius $r_{p}$ and impact parameter $b_p$ of the photon sphere decrease, while the maximum value of effective potential $V_{eff}$ increases. However, as the term $\gamma$ associated with nonlinear electrodynamics increases, the related physical quantities $r_+$, $r_p$ and $b_p$ increase, but the maximum value of $V_{eff}$ decreases. When the light ray reaches the vicinity of the ABG black hole, one can observe the trajectories of the light rays appear as three types, i.e., direct emission, lens ring and photon ring. Furthermore, the shadows and the observational appearance of the ABG black hole are studied. The results show that the charge $q$ and the term $\gamma$ have a great influence on the shape and intensity of the black hole shadow. When the relevant state parameters change or the emission model changes, it can be argued that it is the direct emission that plays a decisive role in the total observed intensity of the ABG black hole, while the contribution of the lens ring to the total observed intensity is small and the photon ring makes almost no contribution.

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Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Shadows and observational appearance of a new family of Ayón-Beato-García black holes

Mou¹,

Chen²,

He³

et al. 2022

Commun. Theor. Phys.

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show abstract

“…Notably, they also showed that the luminosities of both the shadows and rings of the Hayward BH are affected by the accretion flow property and the BH magnetic charge [28]. The BH shadow characteristics in the various gravity are also investigated in [29][30][31][32][33][34][35][36][37].…”

Section: Introductionmentioning

confidence: 99%

QED and accretion flow models effect on optical appearance of Euler–Heisenberg black holes

Zeng

et al. 2022

Eur. Phys. J. C

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Taking the quantum electrodynamics (QED) effect into account, we investigate the geometrical-optics appearance of the Euler–Heisenberg (EH) black hole (BH) under the different accretion flows context, which depends on the BH space-time structure and different sources of light. The more significant magnetic charge leads to the smaller shadow radius for the EH BH, while the different values of the EH parameter do not ruin it. Different features of the corresponding two-dimensional shadow images are derived for the three optically thin accretion flow models. It is shown that the total observed intensity in the static spherical accretion flow scenario leads than that of the infalling spherical accretion flow under same parameters, but the size and position of the EH BH shadows do not change in both of these accretions flows, implying that the BH shadow size depends on the geometric space-time and the shadows luminosities rely on the accretion flow morphology. Of particular interest is that a thin disk accretion model illuminated the BH, we found that the contribution of the lensing ring to the total observed flux is less than $$5\%$$ 5 % , and the photon ring is less than $$2\%$$ 2 % , indicating that the direct emission dominates the optical appearance of the EH BH. It is also believed that the optical appearance of the BH image depends on the accretion disk radiation position in this scenario, which can serve as a probe for the disk structure around the active galactic nucleus (AGN) of M87$$^{*}$$ ∗ like.

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Optical appearance of Einstein-Æther black hole surrounded by thin disk

Cited by 2 publications

References 79 publications

Shadows and observational appearance of a new family of Ayón-Beato-García black holes

Shadows and observational appearance of a new family of Ayón-Beato-García black holes

QED and accretion flow models effect on optical appearance of Euler–Heisenberg black holes

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