The radiation driven winds of rotating B[e] supergiants

We have formulated the momentum equation for sectorial line driven winds fr om rotating stars including: (a) the oblateness of the star, (b) gravity da rkening (von Zeipel effect), (c) conservation of angular momentum, (d) line driving specified by the force multiplier parameters (k, alpha, delta), (e ) finite disk correction factors for an oblate star with gravity darkening for both the continuum and the line driving. The equations are solved numer ically. We calculated the distribution of the mass flux and the wind veloci ty from the pole to the equator for the winds of B[e]-supergiants. Rotation decreases the terminal velocity in the equatorial region but hardly affect s the wind velocity from the poles; it enhances the mass flux from the pole s while the mass flux from the equator remains nearly the same. These effec ts increase with increasing rotation rates. We also calculated models with a bi-stability jump around 25 000 K, using f orce multiplier!; recently calculated with a Monte Carlo technique. In this case the mass flux increases drastically from the pole to the equator and the terminal velocity decreases drastically from pole: to equator. This pro duces a density contrast in the wind rho(equator)/rho(pole) of about a fact or 10 independent of the rotation rate of the star. We suggest that the obs erved density contrast of a factor similar to 10(2) of the disks of B[e] st ars may be reached by taking into account the wind compression due to the t rajectories of the gas above the critical point towards the equatorial plan e.