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We report on simulations in general relativity of magnetized disks onto blackhole binaries. We vary the binary mass ratio from 1:1 to 1:10 and evolve thesystems when they orbit near the binary-disk decoupling radius. We compare(surface) density profiles, accretion rates (relative to a single, non-spinningblack hole), variability, effective $\alpha$-stress levels and luminosities asfunctions of the mass ratio. We treat the disks in two limiting regimes: rapidradiative cooling and no radiative cooling. The magnetic field lines clearlyreveal jets emerging from both black hole horizons and merging into one commonjet at large distances. The magnetic fields give rise to much stronger shockheating than the pure hydrodynamic flows, completely alter the disk structure,and boost accretion rates and luminosities. Accretion streams near the horizonsare among the densest structures; in fact, the 1:10 no-cooling evolutionresults in a refilling of the cavity. The typical effective temperature in thebulk of the disk is $\sim 10^5 (M/10^8 M_\odot)^{-1/4} (L/L_{\rm edd})^{1/4}{\rm K}$ yielding characteristic thermal frequencies $\sim 10^{15} (M/10^8M_\odot)^{-1/4} (L/L_{\rm edd})^{1/4}(1+z)^{-1}{\rm Hz} $. These systems arethus promising targets for many extragalactic optical surveys, such as LSST,WFIRST, and PanSTARRS.

Accretion disks around binary black holes of unequal mass: GRMHD simulations near decoupling