Isothermal two-component stellar wind of hot stars

We present results of the solution of hydrodynamic equations of a two-compo nent radiatively driven stellar wind with an inclusion of the frictional fo rce. The temperature of the wind is assumed to be equal to the effective te mperature of the star. We found that for the case of late B stars the stell ar wind does not decouple, but its terminal velocity is lowered with respec t to the one-component solution. This effect is a consequence of the radiat ive force dependence on the velocity gradient, which is inherent to the CAK model using the Sobolev approximation. For hot B star and O stars there is no significant difference between one a nd two-component solutions.