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

Abstract

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 .

Rotating black holes with an anisotropic matter field

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Multi-level images around Kerr-Newman black holes

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

“…When quantum corrections are taken into account, it turns out that the quantum corrected Schwarzschild black hole has a larger bright lensing ring than that of the classical Schwarzschild one [45]. In addition, f (R) global monopole black hole [46], Kehagias-Sfetsos black hole [47], black bounces [48], noncommutative black hole [49], Brane-World black hole [50], and black hole with torsion charge [51], etc. have been studied by this method.…”