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We use a 3D Monte Carlo radiative transfer code to study the polarimetric andphotometric variability from stationary corotating interaction regions (CIR) inthe wind of massive stars. Our CIRs are approximated by Archimedean spirals ofhigher (or lower) density formed in a spherical wind originating from the starand we also made allowance for a bright gaussian spot at the base of the CIR.Comparing results from our code to previous analytical calculations in theoptically thin case, we find differences which we attribute mainly to a betterestimation of the total unpolarized flux reaching the observer. In theoptically thick case, the differences with the analytical calculations are muchlarger, as multiple scattering introduces extra complexities includingoccultation effects. The addition of a gaussian spot does not alter the shapeof the polarization curve significantly but does create a small excess inpolarization. On the other hand, the effect can be larger on the light curveand can become dominant over the resulting CIR, depending on the spotparameters and density of the wind.

Monte Carlo Simulations of Polarimetric and Light Variability from Corotating Interaction Regions in Hot Stellar Winds