  I start with a discussion of spherical winds and small-scale clumping, before
continuing with various theories that have been proposed to predict how mass
loss depends on stellar rotation -- both in terms of wind strength, as well as
the latitudinal dependence of the wind. This very issue is crucial for our
general understanding of angular momentum evolution in massive stars, and the
B[e] phenomenon in particular. I then discuss the tool of linear polarimetry
that allows us to probe the difference between polar and equatorial mass loss,
allowing us to test B[e] and related disk formation theories.
