Abstract
Through the Blandford-Znajek (BZ) process, a spinning black hole (BH) with a magnetized accretion flow launches relativistic jets -collimated outflows of particles moving at speeds close to the speed of light. These jets are highly energetic and can significantly impact the environment, influencing star formation and galaxy evolution. We conducted general relativistic radiative magnetohydrodynamic (GRRMHD) simulations to investigate the behavior of accretion disks and jets in the regime of super-Eddington magnetically-arrested disks (MAD), an area previously underexplored due to computational limitations. Our simulations reveal a breakdown of the symmetry in jet powers between prograde and retrograde BHs, contrary to predictions from the classical BZ formula, likely linked to the angular frequency of magnetic field lines around the BHs. Additionally, we derived an empirical formula that relates jet power to BH spin and accretion rate, and explored the relations among jet power, magnetic flux, and accretion rate.
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