Mass Transfer in Binary Systems by Stellar Wind

The results of 2D gas-dynamic calculation of mass transfer in binaries with components not filling the Roche lobe are submited. In non-adiabatic gas-dynamic model the various stellar wind velocities were considered. It is shown, that in the case of the small stellar wind velocity values typical for symbiotic stars (comparable with the orbital velocity), two bow shock waves were formed. These shocks are located in front of the accreting star on the way of its orbital movement and between the system components. The steady accreting disk is formed in this case as well. The increasing of the stellar wind velocity results in the transformation of flow structure, formation of conic shock wave, and decreasing of the accretion rate expressed in primary star mass loss rate. The calculated dependence of the theoretical line profiles on the flow structure formed at different stellar wind velocities permits to use the obtained results for observation data interpretation.