We use radiative transfer calculations to reproduce the basic appearance of Mg?II lines observed from Mira variables. These lines have centroids that are blueshifted by at least 30 km?s-1 from the stellar rest frame. It is unlikely that flow velocities in the stellar atmospheres are this fast, so radiative transfer effects must be responsible for this behavior. Published hydrodynamic models predict the existence of cool, downflowing material above the shocked material responsible for the Mg?II emission, and we demonstrate that scattering in this layer can result in Mg?II profiles as highly blueshifted as those that are observed. However, our models also show that scattering within the shock plays an equally strong role in shaping the Mg?II profiles, and our calculations illustrate the importance of partial redistribution and the effects of being out of ionization equilibrium.
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