  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.
