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Employing 3D GRMHD simulation, we study the images of a geometrically thinjet, whose emissions concentrate on its surface, for accretion systemsurrounding a central spinning BH. By introducing a strong magnetic field, weobserve three phases of BH accretion evolution: (a) initially, both theaccretion rate and the magnetic flux on the horizon gradually increase; (b) atan intermediate stage, the magnetic flux approximately reaches saturation, anda jet forms via the Blandford-Znajek (BZ) mechanism; (c) ultimately, the entiresystem achieves a dynamic equilibrium, and a magnetically arrested disk (MAD)forms. We carefully study the jet images during the saturation and MAD regimesat various frequencies and from different observational angles. We reveal thepresence of U-shaped brighter lines near the jet surface boundaries, which canbe attributed to the photons whose trajectories skim over the jet surface. Theexistence of these brighter lines is a unique feature of a geometrically thinjet. Moreover, we notice that the jet images are relatively insensitive to theobserved frequencies of interest. Additionally, we observe that thetime-averaged images for the highly oscillating MAD regime show only slightdifferences from those of the saturation regime.

Imaging a Semi-Analytical Jet model Generated by 3D GRMHD Simulation