A stellar wind model for a magnetic rotating star is presented. We use the semianalytic wind compression model that predicts the two-dimensional geometry of outflows from rotating stars and consider the addition of a magnetic field. In the limit of weak magnetic fields, in such a way that the fields are unimportant in accelerating the flow, the wind compression model can be used to predict the magnetic field distribution throughout the wind, which is shown to follow the mass flux distribution. A compression of field lines near the equator results as the flow of material from higher latitudes brings magnetic flux toward that region. As examples, wind compression models with magnetic fields (“WCField" models)are computed for both a Wolf-Rayet star and a red supergiant star. In both cases an order of magnitude enhancement of the equatorial magnetic field can result within a few stellar radii for stellar rotation rates around 20% of critical. Such enhancements could have consequences for explaining (1) nonthermal emission observed from some Wolf-Rayet winds and (2) the ring structures observed in the ejecta of SN 1987a.