Modeling the Photometric Variability of Alpha² CVn with a Dynamical Magnetosphere

Alpha$^2$ Canum Venaticorum (AM CVn) is a strongly magnetic star with peculiar chemical signatures and periodic variability that have been long attributed to the diffusion of elements through photosphere, leading spots across stellar surface. However, recent studies other hot stars are consistent magnetospheric clouds above Here we take renewed approach modeling AM CVn simplified dynamical magnetosphere (DM) tilted, offset dipole reproduce its Transiting Exoplanet Survey Satellite (TESS) variability. Our model also reproduces well surface map from Silvester, Kochukhov, & Wade (2014). Its ultraviolet variability, IUE archival spectra, traditional reddening models. We further discuss implications on observable quantities system conclude it unlikely be present in CVn.