Abstract
The effects of stellar rotation on the shape of a star are included in the radiation-driven wind theory in order to study their influence upon disk formation in Be stars. For this purpose, we consider a rotationally oblated star and obtain the line force parameters consistently with the hydrodynamic momentum equations. We discuss the influence of the rotation and the bi-stability mechanism in the formation of a two-component wind (fast wind in polar latitudes and slow wind in equatorial regions).
