Abstract
Molecular Clouds (MCs)the birth places of stars – are highly structured and “turbulent”. Converging HI flows have been suggested as a possible generation mechanism of molecular clouds, imprinting the observed filamentary structure as a consequence of dynamical and thermal instabilities. I will discuss a numerical analysis of molecular cloud formation via converging HI flows. Even with modest flow speeds and completely uniform inflows, non-linear density perturbation as possible precursors of MCs arise. Thus, molecular clouds could inevitably be formed with substantial structure, e.g. strong density and velocity fluctuations, which provide the initial conditions for subsequent gravitational collapse and star formation in a variety of galactic and extragalactic environments.
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