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We perform the first suite of fully general relativistic magnetohydrodynamicsimulations of spinning massive black hole binary mergers. We consider binaryblack holes with spins of different magnitudes aligned to the orbital angularmomentum, which are immersed in a hot, magnetized gas cloud. We investigate theeffect of the spin and degree of magnetization (defined through the fluidparameter $\beta^{-1}\equiv p_{\mathrm{mag}}/p_{\mathrm{fluid}}$) on theproperties of the accretion flow. We find that magnetized accretion flows arecharacterized by more turbulent dynamics, as the magnetic field lines aretwisted and compressed during the late inspiral. Post-merger, the polar regionsaround the spin axis of the remnant Kerr black hole are magnetically dominated,and the magnetic field strength is increased by a factor $\sim$10$^2$(independently from the initial value of $\beta^{-1}$). The magnetized gas inthe equatorial plane acquires higher angular momentum, and settles in a thincircular structure around the black hole. We find that mass accretion rates ofmagnetized configurations are generally smaller than in the unmagnetized casesby up to a factor $\sim$3. Black hole spins have also a suppressing effect onthe accretion rate, as large as $\sim$48\%. As a potential driver forelectromagnetic emission we follow the evolution of the Poynting luminosity,which increases after merger up to a factor $\sim2$ with increasing spin,regardless of the initial level of magnetization of the fluid. Our resultsstress the importance of taking into account both spins and magnetic fieldswhen studying accretion processes onto merging massive black holes.

Fully General Relativistic Magnetohydrodynamic Simulations of Accretion Flows onto Spinning Massive Black Hole Binary Mergers