INFLUENCE OF BOUNDARY PARAMETERS OF THE S TELLAR WIND ON THE STRUCTURE OF THE FLOW OF MATTER IN BINARIES WITH COMPONENTS THAT ARE NOT FILLING THEIR ROCHE LOBE

Results of two-dimensional gas dynamic computations of flow of matter in binaries are presented. They illustrate characteristic features of the flow and the influence of boundary parameters of the stellar wind on the structure of the flow. It is shown, that if the losing mass pri mary is not filling its Roche lobe, the structure of the flow is deter mined not only by the mass flow through the vicinity of the internal L agrangian point L1, but also by the flow of matter caused by orbital m otion of the secondary (the accreting component) through the gas lost by the primary. Our computations reveal a complicated structure of the flow consisting of shock waves and tangential breaks, with several pe culiarities. For all computed versions a detached shock wave is presen t in the flow in front of the compact secondary along the orbital moti on, and another detached shock wave between the components of the bina ry. The physical parameters of the stellar wind influence substantial the structure of the flow of matter. It is shown, that accretion on th e secondary has a spiral feature. The boundaries of this spiral betwee n the components are shock waves; above and below the flow the boundar ies are tangential breaks. An instability of the accretion process rev ealed in the computations is discussed.