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Recent large-scale spectropolarimetric surveys have established that a smallbut significant percentage of massive stars host stable, surface dipolarmagnetic fields with strengths on the order of kG. These fields channel thedense, radiatively driven stellar wind into circumstellar magnetospheres, whosedensity and velocity structure can be probed using ultraviolet (UV)spectroscopy of wind-sensitive resonance lines. Coupled with appropriatemagnetosphere models, UV spectroscopy provides a valuable way to investigatethe wind-field interaction, and can yield quantitative estimates of the windparameters of magnetic massive stars. We report a systematic investigation ofthe formation of UV resonance lines in slowly rotating magnetic massive starswith dynamical magnetospheres. We pair the Analytic Dynamical Magnetosphere(ADM) formalism with a simplified radiative transfer technique to producesynthetic UV line profiles. Using a grid of models, we examine the effect ofmagnetosphere size, the line strength parameter, and the cooling parameter onthe structure and modulation of the line profile. We find that magnetic massivestars uniquely exhibit redshifted absorption at most viewing angles andmagnetosphere sizes, and that significant changes to the shape and variation ofthe line profile with varying line strengths can be explained by examining theindividual wind components described in the ADM formalism. Finally, we showthat the cooling parameter has a negligible effect on the line profiles.

Ultraviolet Line Profiles of Slowly Rotating Massive Star Winds Using the "Analytic Dynamical Magnetosphere" Formalism