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

Abstract

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 upon a new slow solution for different high rotational radiation driven winds (Curé 2004) 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.

5 pages, 5 figures, Accepted for publication in Astronomy & Astrophysics

References in corpus (4)

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• On the optical--infra-red continuum emission from equatorial discs of supergiant B[e] stars
• The ionization structure of early-B supergiant winds
• The influence of rotation in radiation driven winds from hot stars II. CAK topological analysis

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