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We perform magnetohydrodynamic simulations of accreting, equal-mass binaryblack holes in full general relativity focusing on the impact of black holespin on the dynamical formation and evolution of minidisks. We find that duringthe late inspiral the sizes of minidisks are primarily determined by theinterplay between the tidal field and the effective innermost stable orbitaround each black hole. Our calculations support that a minidisk forms when theHill sphere around each black hole is significantly larger than the blackhole's effective innermost stable orbit. As the binary inspirals, the radius ofthe Hill sphere decreases, and minidisk sconsequently shrink in size. As aresult, electromagnetic signatures associated with minidisks may be expected togradually disappear prior to merger when there are no more stable orbits withinthe Hill sphere. In particular, a gradual disappearance of a hardelectromagnetic component in the spectrum of such systems could provide acharacteristic signature of merging black hole binaries. For a binary of giventotal mass, the timescale to minidisk "evaporation" should therefore depend onthe black hole spins and the mass ratio. We also demonstrate that accretingbinary black holes with spin have a higher efficiency for converting accretionpower to jet luminosity. These results could provide new ways to estimate blackhole spins in the future.

Minidisk dynamics in accreting, spinning black hole binaries: Simulations in full general relativity