  We have formulated the momentum equation for sectorial line driven winds from
rotating stars including: (a) the oblateness of the star, (b) gravity darkening
(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 numerically. We
calculated the distribution of the mass flux and the wind velocity from the
pole to the equator for the winds of B[e]-supergiants. Rotation decreases the
terminal velocity in the equatorial region but hardly affects the wind velocity
from the poles; it enhances the mass flux from the poles while the mass flux
from the equator remains nearly the same. These effects increase with
increasing rotation rates.
  We also calculated models with a bi-stability jump around 25 000 K, using
force multipliers 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 produces a
density contrast in the wind rho(equator/pole) of about a factor 10 independent
of the rotation rate of the star. We suggest that the observed density contrast
of a factor 100 of the disks of B[e] stars may be reached by taking into
account the wind compression due to the trajectories of the gas above the
critical point towards the equatorial plane.
