STRUCTURE OF THE ACCRETION DISK IN SYMBIO TIC STARS - THE ISOTHERMAL CASE

Results of two-dimensional gas dynamic computations of gas flow in sym biotic stars are presented with radiation cooling of gas in the formin g accretion disk taken into consideration. As computations show radiat ion cooling does not change qualitatively the picture of the flow in v icinity of the accreting star. The structure of the accretion disk wit h lagging and leading spiral shock waves remains also unchanged. Radia tion cooling affects to a great extent numerical values of parameters of the flow. So the coefficient of accretion efficiency increases from 0.15 to 0.8. It is shown that alteration of parameters of the binary are not influencing significantly the picture of the flow and the stru cture of the accretion disk. Therefore, the computed structure of the flow seems to be typical for symbiotic stars.