  We present the results of three-dimensional numerical simulations of mass
transfer in semi-detached binary systems in which the mass-losing star is
rotating. The cases of aligned and misaligned non-synchronous rotation of the
donor star are considered; the resulting flow patterns are compared to the
synchronous case. The main properties of the flow, such as the formation of an
circumbinary envelope, the absence of a "hot spot" on the edge of the accretion
disk, and the formation of a shock wave along the flow edge, are qualitatively
similar to those obtained earlier. For the case of misaligned, non-synchronous
rotation, the behavior of the disk and surrounding matter in established flow
regime reflects changes in the boundary conditions at the surface of the donor
star; in other words, a "driven disk" model is realized in the calculations.
