The impact of the slow solutions in the winds of massive stars
The standard theory that describe the wind of massive stars is the
radiation driven wind model from Castor et al. (CAK 1975).
When the influence of the stellar rotation is included, besides the standard
solution of the CAK wind there also exists a new
wind solution that we called the slow-omega solution (Curé 2004).
We have already successfully described the two component wind of B[e]
supergiants (Curé et al. 2005).
Furthermore we apply this two component model for a classical Be stars with
an oblate structure to describe the winds of
these objects, explaining the observed contrast in density between
equatorial and polar densities.
Another slow solution exists when the line force parameter delta is larger
than ~0.25, we call this the slow-delta solution,
which has a slower terminal velocity and lower mass loss rate than the fast
solution.
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