Shadows and photon spheres with spherical accretions in the four-dimensional Gauss–Bonnet black hole

Zeng, Xiao-Xiong; Zhang, Haiqing; Zhang, Hongbao

doi:10.1140/epjc/s10052-020-08449-y

Cited by 158 publications

(75 citation statements)

References 26 publications

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“…Interestingly, the solution of the same form has been presented in the conformal anomaly inspired gravity [40,41]. Along this line, the Einstein-Gauss-Bonnet gravity in the 4D spacetime has been explored extensively on various aspects, including the exact solutions [42][43][44][45][46][47][48][49][50][51][52][53][54][55], the quasinormal modes and stability [56][57][58][59][60][61][62][63][64][65][66][67], the observable shadows [68][69][70][71][72][73], the geodesics and gravitational lensing [74][75][76][77][78], and the thermodynamics and cosmic censorship conjecture [79][80][81][82][83][84][85][86].…”

Section: Jhep12(2020)192mentioning

confidence: 99%

Holographic superconductors in 4D Einstein-Gauss-Bonnet gravity

Qiao

Ouyang

Wang

et al. 2020

J. High Energ. Phys.

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We investigate the neutral AdS black-hole solution in the consistent D → 4 Einstein-Gauss-Bonnet gravity proposed in [K. Aoki, M.A. Gorji, and S. Mukohyama, Phys. Lett. B810 (2020) 135843] and construct the gravity duals of (2 + 1)-dimensional superconductors with Gauss-Bonnet corrections in the probe limit. We find that the curvature correction has a more subtle effect on the scalar condensates in the s-wave superconductor in (2 + 1)-dimensions, which is different from the finding in the higher-dimensional superconductors that the higher curvature correction makes the scalar hair more difficult to be developed in the full parameter space. However, in the p-wave case, we observe that the higher curvature correction always makes it harder for the vector condensates to form in various dimensions. Moreover, we note that the higher curvature correction results in the larger deviation from the expected relation in the gap frequency ωg/Tc ≈ 8 in both (2 + 1)-dimensional s-wave and p-wave models.

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Section: Jhep12(2020)192mentioning

confidence: 99%

Holographic superconductors in 4D Einstein-Gauss-Bonnet gravity

Qiao

Ouyang

Wang

et al. 2020

J. High Energ. Phys.

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“…In this case, the optical appearance of shadow with two photon spheres in a Hairy Black Hole has been presented in [78], where the smaller photon sphere is considered to be the shadow boundary. For another model of accretion, namely the optically thin and geometrically thin disk, the later studies [79][80][81][82][83][84][85][86][87] show that the size of shadow is closely related to the position of the accretion, and the bright region outside of shadow are always composed of direct emission, lensing rings and photon rings. With this consideration, an optically observational signature of the asymmetric thin-shell wormhole has been thoroughly investigated, which shows that this signature can be used to distinguish wormholes from black holes [88].…”

Section: Introductionmentioning

confidence: 99%

Observational appearances of a f(R) global monopole black hole illuminated by various accretions

2021

Eur. Phys. J. C

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In this paper, we explore three simple models of accretions on a global monopole black hole in f(R) theory, and numerically study the corresponding observational appearances as seen by an observer located at the asymptotic infinity and the certain region out of black hole. For the thin-disk accretion, the results here show that the brighter lensing ring and the darker photon ring that around black hole shadow, always make a small contribution and a negligible contribution to total observed intensity respectively. While, the direct emission of disk contributes a dominant part, and the size of shadow always depends on the disk’s location. For the static and infalling spherical accretions, it turns out that the radiuses of the shadows and photon spheres are always same for both accretions, which implies that the boundary of shadow represents the signature of the spacetime geometry in this case. However, we also find that the brightness of shadow in infalling accretion is darker than that in static case since the Doppler effect is taken into account. In addition, the effect of the global monopole parameter $$\eta $$ η and f(R) parameter $$\psi _0$$ ψ 0 on observational appearances of black hole are clearly emphasized throughout of this paper. Finally, we conclude that black hole shadows and the related rings with some different observable features can be used for us to distinguish black holes from different gravity theories and set the upper limits to the f(R) parameter $$\psi _0$$ ψ 0 .

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“…The physical properties and the novel observable a e-mail: csb3752@hunnu.edu.cn (corresponding author) b e-mail: jljing@hunnu.edu.cn effects for these black hole solutions have been explored in Refs. [2][3][4][5][6][7]. However, there are also some criticisms on this theory of Gravity [8][9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

Tidal effects in 4D Einstein–Gauss–Bonnet black hole spacetime

Chen

Jing

2021

Eur. Phys. J. C

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We have investigated tidal forces and geodesic deviation motion in the 4D-Einstein–Gauss–Bonnet spacetime. Our results show that tidal force and geodesic deviation motion depend sharply on the sign of Gauss–Bonnet coupling constant. Comparing with Schwarzschild spacetime, the strength of tidal force becomes stronger for the negative Gauss–Bonnet coupling constant, but is weaker for the positive one. Moreover, tidal force behaves like those in the Schwarzschild spacetime as the coupling constant is negative, and like those in Reissner–Nordström black hole as the constant is positive. We also present the change of geodesic deviation vector with Gauss–Bonnet coupling constant under two kinds of initial conditions.

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Shadows and photon spheres with spherical accretions in the four-dimensional Gauss–Bonnet black hole

Cited by 158 publications

References 26 publications

Holographic superconductors in 4D Einstein-Gauss-Bonnet gravity

Holographic superconductors in 4D Einstein-Gauss-Bonnet gravity

Observational appearances of a f(R) global monopole black hole illuminated by various accretions

Tidal effects in 4D Einstein–Gauss–Bonnet black hole spacetime

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