"WCFields": A magnetic rotating stellar wind model from wind compression theory

A stellar wind model for a magnetic rotating star is presented. We use the semianalytic wind compression model that predicts the two-dimensional geome try of outflows from rotating stars and consider the addition of a magnetic held. 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 line s near the equator results as the flow of material from higher latitudes br ings magnetic flux toward that region. As examples, wind compression models with magnetic fields ('"WCField" models) are computed fur both a Wolf-Raye t star and a red supergiant star. In both cases an order of magnitude enhan cement of the equatorial magnetic held can result within a few stellar radi i for stellar rotation rates around 20% of critical. Such enhancements coul d have consequences for explaining (1) nonthermal emission observed from so me Wolf-Rayet winds and (2) the ring structures observed in the ejecta of S N 1987a.