  Massive star winds are structured both stochastically ("clumps") and often
coherently (Co-rotation Interaction Regions, or CIRs). Evidence for CIRs
threading the winds of Wolf-Rayet (WR) stars arises from multiple diagnostics
including linear polarimetry. Some observations indicate changes in
polarization position angle across optical recombination emission lines from a
WR star wind but limited to blueshifted Doppler velocities. We explore a model
involving a spherical wind with a single conical CIR stemming from a rotating
star as qualitative proof-of-concept. To obtain a realistic distribution of
limb polarization and limb darkening across the pseudo-photosphere formed in
the optically thick wind of a WR star, we used Monte Carlo radiative transfer
(MCRT). Results are shown for a parameter study. For line properties similar to
WR 6 (EZ CMa; HD 50896), the combination of the MCRT results, a simple model
for the CIR, and the Sobolev approximation for the line formation, we were able
to reproduce variations in both polarization amplitude and position angle
commensurate with observations. Characterizing CIRs in WR~winds has added
importance for providing stellar rotation periods since the v sin i values are
unobtainable because the pseudo-photosphere forms in the wind itself.
