Synthetic molecular clouds from supersonic MHD and non-LTE radiative transfer calculations

The dynamics of molecular clouds is characterized by supersonic random motions in the presence of a magnetic field. We study this situation using numerical solutions of the three-dimensional compressible magnetohydrodynamic (MHD) equations in a regime of highly supersonic random motions. The non-LTE radiative transfer calculations are performed through the complex density and velocity fields obtained as solutions of the MHD equations, and more than 5 x 10(5) spectra of (CO)-C-12, (CO)-C-13, and CS are obtained. In this way we build synthetic molecular clouds of 5 and 20 pc diameter, evolved for about one dynamical time from their initial cofiguration. We use a numerical flow without gravity or external forcing. The flow is super-Alfvenic. Synthetic data consist of sets of 90 x 90 synthetic spectra with 60 velocity channels, in five molecular transitions: J=1-->0 and J=2-->1 for (CO)-C-12 and (CO)-C-13 and J=1-->0 for CS. Although we do not consider the effects of stellar radiation, gravity, or mechanical energy input from discrete sources, our models do contain the basic physics of magneto fluid dynamics and non-LTE radiation transfer and are therefore more realistic than previous calculations. As a result, these synthetic maps and spectra bear a remarkable resemblance to the corresponding observations of real clouds.