vendredi 11 février 2011, par Michel Curé (Université de Valparaiso, Chili)
Mardi 22 mars 2011 à 11h00 , Lieu : Salle de confĂ©rence du bât. 17
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 de 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.
We have successfully applied this new slow-delta solution to explain the winds of A-Supergiants and we believe this solution can solve the weak wind problem. Finally we discuss the impact of this new slow-delta solution in the WML relationship.
