Cure et al. (2005) revisited radiative driven wind models for rapidly rotating B[e] supergiants, assuming a change in the line-force parameters due to the hi-stability jump. From their model calculations, they made predictions on the density contrast close and far from the star and also the disk half-opening angle. In that work they neglected the effect of rotation in the shape of the star and also in the finite- disk correction factor. In the present work, we present our first steps in the study of the influence of the oblate finite disk correction factor due to rotation (Pelupessy et al. 2000) in the wind solutions.