Determination of magnetic fields in the winds from hot stars using the Hanle effect

Resonance lines that are sensitive to the Hanle effect are prominent in the UV spectra of early-type stars. To understand the differences from the solar application of the Hanle effect, we focus on the formation of P-Cygni lines both as a scattering process, and as one that allows a spectral isolation of sectors in the wind. Some complications occuring in the solar case are found to be absent for the Hanle effect for hot stars, Rocket observations from the Far Ultraviolet SpectroPolarimeter (FUSP) experiment should allow for a determination of fields in the dynamically interesting range from 1 to 300 Gauss.