The effect of the normal star on the compact magnetized component is
largely determined by the rate
and velocity of stellar wind at infinity
. For the majority of cases, we assume

where
is the parabolic velocity at the stellar surface.

For Be-stars (i.e. those stars at the stage ``I'' whose mass increased
during the first mass exchange), the wind velocity at infinity is taken
to be equal to the Keplerian velocity at the stellar
surface

Thus, the lower stellar wind velocity leads to an effective increase
of the captured mass rate by a secondary companion to such Be-stars.

The stellar wind rate at stage ``I'' is calculated as (de Jager 1980[41])

Here
is a numerical coefficient.

For giant post-MS stars (stage ``II''), we assume
and for massive star we take maximum wind rate between that given by de
Jager's formula and that given by Lamers (1981)[94]:

For red supergiants at the asymptotic giant branch (AGB) stage, we use
Reimers's formula (Kudritzki and Reimers, 1978[88])

When a massive star becomes a Wolf-Rayet star, its stellar wind can
significantly increase (up to
yr
). We parametrize such a wind as