Bistability rotating radiation driven wind for B[e] Supergiants: the oblate finite cone angle correction factor.

GRANADA, A.; JIMENEZ, A.; CURE, M.; CIDALE, L.

Santiago de Chile, Chile

Workshop; The Interferometric View on Hot Stars, Eds. Th. Rivinius & M. Curé; 2009

Cure et al. (2005) revisited radiative driven wind models for rapidly rotating B[e] supergiants, assuming a change in the line-force parameters due to the bi-stability jump. From their model calculations, they made predictions on the density contrast close and far from the star and also the disk half-opening angle. In that work they neglected the efect of rotation in the shape of the star and also in the nite- disk correction factor. In the present work, we present our rst steps in the study of the inuence of the oblate nite disk correction factor due to rotation (Pelupessy et al. 2000) in the wind solutions.