X-RAY LIGHT CURVES IN A MODEL FOR COLLIDI NG STELLAR WINDS IN CLOSE BINARY-SYSTEMS - APPLICATION TO SS 433

A method for the calculation of the X-ray light curves of close binary systems is proposed, based pn a model for the collision of stellar wi nds. The source of X-ray radiation is gas emitting between two fronts near the collision of flows from components of the system. The light c urve is caused by the eclipse of part of the emitting surface by the s tars in their orbital rotation. The shape of the theoretical light cur ve depends significantly on fundamental parameters of the system: the distance between components, the diameters of the stars, their effecti ve temperatures, the flow rate and wind speed for each component. Comp arison of theoretical and observed light curves permits, in principle, refinement of some parameters of close binary systems. The method Is used to interpret the light curve of SS 433 in the energy range from 6 to 30 keV.