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Isothermal two-component stellar wind of hot stars
Received 13 December 1999 / Accepted 22 May 2000
We present results of the solution of hydrodynamic equations of a two-component radiatively driven stellar wind with an inclusion of the frictional force. The temperature of the wind is assumed to be equal to the effective temperature of the star. We found that for the case of late B stars the stellar wind does not decouple, but its terminal velocity is lowered with respect to the one-component solution. This effect is a consequence of the radiative 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 and two-component solutions.
Key words: stars: mass-loss stars: winds, outflows hydrodynamics stars: early-type
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Online publication: July 13, 2000