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The study of Magnetically Arrested Disks (MAD) attract strong interest inrecent years, as these disk configurations were found to generate strong jetsas observed in many accreting systems. Here, we present the results of 14general relativistic magnetohydrodynamic(GRMHD) simulations of advectiondominated accretion flow in the MAD state across black hole spins, carried withcuHARM. Our main findings are as follows. (i) The jets transport a significantamount of angular momentum to infinity in the form of Maxwell stresses. Forpositive, high spin, the rate of angular momentum transport is about 5 timeslarger than for negative spin. This contribution is nearly absent for anon-rotating black hole. (ii) The mass accretion rate and the MAD parameter,both calculated at the horizon, are not correlated. However, their timederivatives are anti-correlated for every spin. (iii) For zero spin, thecontribution of the toroidal component of the magnetic field to the magneticpressure is negligible, while for fast spinning black hole, it is in the sameorder as the contribution of the radial magnetic component. For high positivespin, the toroidal component even dominates. (iv) For negative spins, the jetsare narrower than their positive spin counterparts, while their fluctuationsare larger. The weak jet from the non-rotating black hole is the widest withthe smallest fluctuations. Our results highlight the complex, non-linearconnection between the black hole spin and the resulting disk and jetproperties in the MAD regime.

A study of the MAD accretion state across black hole spins for radiatively inefficient accretion flows