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

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.