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

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

2005-03-16

arxiv.org/abs/astro-ph/0503359v1

Astronomy and Astrophysics

Astrophysics

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

Scientific paper

10.1051/0004-6361:20052686

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 (Cur\'e 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.

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