Abstract
The ISM shock waves due to the collisions of a high velocity cloud (HVC) and the galactic disk can generate turbulence and star formation processes. As a particular feature, a fraction of gas is ejected out of the disk, and this could be the origin of some molecular complexes like the Chamaeleon andrho Ophiuchi clouds. One can observe some hydrodynamical phases during the shock, when the cloud presents a coalescence stage, followed by re-expansion and deep disk penetration. We present results of evolving shocks done by 3D hydrodynamical simulations of a falling high velocity cloud on the galactic disk with conditions more realistic than preceding studies, with equations which include molecular cooling.
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Work supported by CNPq grant process 201793/92-0
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Hetem, A. Shocks of high velocity clouds and the galactic disk. Astrophys Space Sci 233, 181–184 (1995). https://doi.org/10.1007/BF00627348
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DOI: https://doi.org/10.1007/BF00627348