MATTER EXCHANGE IN BINARIES VIA STELLAR W IND

The results of two-dimensional gas dynamical calculations of matter ex change in binaries with components that do not fill their Roche lobes are presented. Various stellar wind velocity regimes are considered in the framework of a nonadiabatic gas dynamical model. It is shown that for the small wind velocities typical of symbiotic stars (comparable to the orbital velocity), a stable accretion disk and two outwardly di rected shock waves form: one in front of the accretor on the path of t he orbital motion and the second between the components of the system. Increasing the stellar wind velocity leads to the transformation of t he flow and the formation of a conical shock. Increasing the wind velo city also reduces the ratio of the gas accretion rate to the mass loss rate of the primary. The calculated changes in the flow pattern as a function of the stellar wind velocity substantially affect the shapes of the emission line profiles, and therefore can be used in the interp retation of observational data.