  Recent large-scale spectropolarimetric surveys have established that a small
but significant percentage of massive stars host stable, surface dipolar
magnetic fields with strengths on the order of kG. These fields channel the
dense, radiatively driven stellar wind into circumstellar magnetospheres, whose
density and velocity structure can be probed using ultraviolet (UV)
spectroscopy of wind-sensitive resonance lines. Coupled with appropriate
magnetosphere models, UV spectroscopy provides a valuable way to investigate
the wind-field interaction, and can yield quantitative estimates of the wind
parameters of magnetic massive stars. We report a systematic investigation of
the formation of UV resonance lines in slowly rotating magnetic massive stars
with dynamical magnetospheres. We pair the Analytic Dynamical Magnetosphere
(ADM) formalism with a simplified radiative transfer technique to produce
synthetic UV line profiles. Using a grid of models, we examine the effect of
magnetosphere size, the line strength parameter, and the cooling parameter on
the structure and modulation of the line profile. We find that magnetic massive
stars uniquely exhibit redshifted absorption at most viewing angles and
magnetosphere sizes, and that significant changes to the shape and variation of
the line profile with varying line strengths can be explained by examining the
individual wind components described in the ADM formalism. Finally, we show
that the cooling parameter has a negligible effect on the line profiles.
