Abstract

My abstract is  "Quasi-molecular resonances are spectral features that form due to transient close collisions between neighboring plasma particles in hot dense plasmas. The UV spectra of white dwarf stars is particularly sensitive to Lyman-series H2+ quasi-molecular resonances, and the modeling of these features can substantially impact white dwarf stellar parameter fits. In this talk we present a novel method for calculating atomic spectral line shape profiles with H2+ resonances included, using a new change-of-basis approach. With this treatment we have removed a number of physical approximations that have previously been relied upon, including the binary collision approximation. We show new hydrogen Lyman-α profiles calculated with this method and discuss some of the differences compared to past theory. Finally we highlight this method’s rather unique treatment of radiator unitarity and possible applications to future opacity calculations.