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 as a result of stream-disk shocks driven by the binary torques .