  When an accretion disk surrounds a binary rotating in the same sense, the
binary exerts strong torques on the gas. Analytic work in the 1D approximation
indicated that these torques sharply diminish or even eliminate accretion from
the disk onto the binary. However, recent 2D and 3D simulational work has shown
at most modest diminution. We present new MHD simulations demonstrating that
for binaries with mass ratios of 1 and 0.1 there is essentially no difference
between the accretion rate at large radius in the disk and the accretion rate
onto the binary. To resolve the discrepancy with earlier analytic estimates, we
identify the small subset of gas trajectories traveling from the inner edge of
the disk to the binary and show how the full accretion rate is concentrated
onto them.
