Outflowing disk formation in B[e] supergiants due to rotation and bi-stability in radiation driven winds

Michel Curé (1), Diego F. Rial (2) and Lydia Cidale (3)

(1) Departamento de Física y Meteorología, Facultad de Ciencias, Universidad de Valparaíso, Chile
(2) Departamento de Matemáticas, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina
(3) Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, La Plata, Buenos Aires, Argentina.

The effects of rapid rotation and bi-stability upon the density contrast between the equatorial and polar directions of a B[e] supergiant are re-investigated. Based on a new slow solution for different high rotational radiation-driven winds and the fact that bi-stability allows a change in the line--force parameters ($\alpha$, $k$, and $\delta$), the equatorial densities are about $10^2$--$10^4$ times higher than the polar ones. These values are in qualitative agreement with the observations.

Reference: Cure, M., Rial, D. F. and Cidale, L., Astronomy and Astrophysics, in press
Status: Manuscript has been accepted



Email: michel.cure@uv.cl