Obtained values of coincide well with the characteristic value of this quantity for supergiants of early spectral classes: (de Jager 1980). We also use well known equation for a terminal velosity of a stellar wind which is well confirmed by observations:
where is the escaping velocity on the surface of the star, We use this dependence and equation (de Jager 1980):
where .
For optical component of GX 301-2 we have: and e=0.47 (Watson et al 1982). We took because in our calculations we used maximum luminosity, i.e. luminosity in periastr. For these values we have: and for we have (for , B1 Iab, in de Jager (1980) we can find ).
From eq. (18) we get:
It coincides well with our maximum value (see table 3).
For Vela X-1 there are such estimates (Haberl 1991): and . We get: It also
coincides with our estimates of the maximum stellar wind velocity:
With different assumptions for the turbulent velocity
(for example ) we can get excellent coincidence of our
results
with the stellar wind velocities estimated above using other techniques.
Acknowledgements.
We thank M.E.Prokhorov for helpful discussions and unknown referees
for there comments.