Abstract

White dwarfs are the final stage of evolution for the majority of all stars in the Milky Way. Accurately determining the parameters of these stars with the widely used spectral fitting method relies heavily on the theoretical spectral line shapes in the model atmospheres. The Xenomorph code, developed by Gomez et al. 2016 and Cho et al. 2022, has made several improvements to theoretical neutral Hydrogen line shapes, but was previously incapable of generating other lines relevant to white dwarf atmospheres. The hot DQ class white dwarf, with dominating C II absorption lines, is theorized to be the result of double-degenerate (D-D) mergers. Mass estimates are needed to better characterize the D-D merger rate of the milky way, but the current state-of-the-art C II line shapes contain approximations that break down in these dense regimes. This, along with the DO class with strong He II absorption lines, has made clear the importance of updating the Xenomorph code to treat charged radiators. By giving the plasma particles hyperbolic trajectories around the radiator, the code will more accurately capture the physics in the line shapes. In the future, these grids of C II and He II lines will be included in model atmosphere codes to fit both laboratory and white dwarf spectra.