  As the disk formation mechanism(s) in Be stars is(are) as yet unknown, we
investigate the role of rapidly rotating radiation-driven winds in this
process. We implemented the effects of high stellar rotation on m-CAK models
accounting for: the shape of the star, the oblate finite disk correction
factor, and gravity darkening. For a fast rotating star, we obtain a
two-component wind model, i.e., a fast, thin wind in the polar latitudes and an
$\Omega$-slow, dense wind in the equatorial regions. We use the equatorial mass
densities to explore H$\alpha$ emission profiles for the following scenarios:
1) a spherically symmetric star, 2) an oblate shaped star with constant
temperature, and 3) an oblate star with gravity darkening. One result of this
work is that we have developed a novel method for solving the gravity darkened,
oblated m-CAK equation of motion. Furthermore, from our modeling we find a) the
oblate finite disk correction factor, for the scenario considering the gravity
darkening, can vary by at least a factor of two between the equatorial and
polar directions, influencing the velocity profile and mass-loss rate
accordingly, b) the H$\alpha$ profiles predicted by our model are in agreement
with those predicted by a standard power-law model for following values of the
line-force parameters: $1.5 \lesssim k \lesssim 3$, $ \, \alpha \sim 0.6$ and
$\, \delta \gtrsim 0.1$, and c) the contribution of the fast wind component to
the H$\alpha$ emission line profile is negligible; therefore, the line profiles
arise mainly from the equatorial disks of Be stars.
