Abstract

The life cycles of massive stars are ultimately linked to their capacity (or incapacity) to retain their mass during their evolution. Their extreme radiation is strong enough to drive mass off their surfaces in a stellar wind, which can be studied using ultraviolet (UV) spectra. Magnetic massive stars, a subset of the OBA -type star population, have surface dipolar magnetic fields about a thousand times stronger than that of the Sun. These fields channel the stellar wind into structurally complex magnetospheres, creating spectral line profiles with atypical shapes. UV resonance lines reveal the density and velocity structure of the magnetosphere and allow us to study the wind/field interaction. To date, large-scale modeling of this phenomenon has been limited by the computational cost. Our analysis, the UV-ADM project, solves this problem by applying a simple analytic prescription to efficiently calculate synthetic UV spectral lines. Our models can be compared to UV observations of magnetic massive stars, enabling us to make better predictions of stellar wind parameters.