  We present the results of three-dimensional numerical simulations of mass
transfer in semi-detached binary with a donor star whose rotation vector
precesses around the orbital rotation axis of the binary in the observer's
coordinate frame. The calculations support our previous model of flow without a
`hot spot'. Characteristic features of the flow in this model, such as the
formation of an circumbinary envelope, the absence of a `hot spot' at the edge
of the accretion disk, and the formation of a shock wave along the edge of the
stream, are also present in the solution for a binary with precessing donor
star. The parameters of accretion disk and of the structure of the near-disk
regions recur with the precessional period of the rotation axis of donor star.
