  The topic of wind-clumping has been the subject of much activity in recent
years, due to the impact that it can have on derived mass-loss rates. Here we
present an alternative method of investigating wind-clumping, that of
polarimetry. We present simulations of the polarization produced by a clumpy
wind, and argue that the observations may be reproduced just by statistical
deviations from spherical symmetry when the outflow is only slightly
fragmented. Here, the polarization scales with $\dot{M}$, which is consistent
with observations of LBVs, WRs and O supergiants. Finally, we find clumping
factors in the inner 2$R_{\star}$ of $\sim 2-3$, and speculate as to the
clumping stratification of hot stars.

Astrophysics