Abstract
The structure of the atmospheres of cool, pulsating stars differs considerably from hydrostatic or stationary states due to the presence of shock waves. Dynamic model calculations that include a detailed description of dust formation predict a more or less complex spatial structure of the circumstellar dust shell on relatively small scales, which is due to the complicated, time-dependent interactions between gas dynamics, dust formation, and radiation. The structure of the atmosphere obtained from dynamic models results in various observable features like spectral energy distributions (Windsteig et al. 1997), spatial brightness profiles, line profiles, and molecular spectra (Loidl et al. 1997). In this contribution we present synthetic CO line profiles based on the models of Hofner & Dorfi (1997).
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