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We perform a full 3D general relativistic magnetohydrodynamical (GRMHD)simulation of an equal-mass, spinning, binary black hole approaching merger,surrounded by a circumbinary disk and with mini-disks around each black hole.For this purpose, we evolve the ideal GRMHD equations on top of an approximatedspacetime for the binary that is valid in every position of space, includingthe black hole horizons, during the inspiral regime. We use relaxed initialdata for the circumbinary disk from a previous long-term simulation, where theaccretion is dominated by an $m=1$ overdensity called the lump. We compare ournew spinning simulation with a previous non-spinning run, studying how spininfluences the mini-disk properties. We analyze the accretion from the inneredge of the lump to the black hole, focusing on the angular momentum budget ofthe fluid around the mini-disks. We find that mini-disks in the spinning casehave more mass over a cycle than the non-spinning case. However, in both cases,we find most of the mass received by the black holes is delivered by the directplunging of material from the lump. We also analyze the morphology andvariability of the electromagnetic fluxes and we find they share the sameperiodicities of the accretion rate. In the spinning case, we find that theoutflows are $8$ times stronger than the non-spinning case. Our results will beuseful to understand and produce realistic synthetic light curves and spectra,which can be used in future observations.

Mini-disk accretion onto spinning black hole binaries: quasi-periodicities and outflows