Originating in different depths of the very extended atmospheres of AGB
stars, various molecular spectral lines observable in the near-infrared show
diverse behaviours and can be used to probe atmospheric dynamics throughout the
outer layers of these pulsating red giants. In Nowotny et al. (2005, Paper I)
time series of synthetic high-resolution spectra were presented, computed from
a dynamic model atmosphere for a typical carbon-rich Mira. In this work, line
profile shapes, their variations during the lightcycle and radial velocities
derived from wavelength shifts are analyzed and compared with results from
observed FTS spectra of the C-rich Mira S Cep and other Miras. It is found that
the global velocity structure of the model is in qualitative agreement with
observations. Radial velocities of molecular lines sampling different layers
behave comparably, although some differences are apparant concerning absolute
values. A correction factor of p=1.36 between measured RVs and actual gas
velocities is derived for CO dv=3 lines. It is shown that dynamic model
atmospheres are capable of reproducing Mira spectra without introducing an
additional ''static layer'' proposed by several authors.Comment: accepted by A&A, 12 pages, 10 figure