Abstract
We simulated collisions of High Velocity Clouds with the galactic disk with a simple hydrodynamical code. Main aspects of the morphology of nearby (d < 500 pc) cloud complexes, like the ρ Oph, Orion and Taurus-Auriga-Perseus complexes, are reproduced. These aspects include total mass, distance from the galactic plane, orientation of elongated gas structures with respect to the plane, and relative position of clusters of O-B stars with respect to the main concentrations of molecular gas. The space distribution of stars of different ages, usually explained in terms of sequential star formation, is interpreted in a new way in our model.
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© 1994 Springer Science+Business Media Dordrecht
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Lépine, J.R.D., Duvert, G. (1994). Are Molecular Clouds Formed by Impact of High-Velocity Clouds?. In: Epchtein, N., Omont, A., Burton, B., Persi, P. (eds) Science with Astronomical Near-Infrared Sky Surveys. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-0946-8_42
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DOI: https://doi.org/10.1007/978-94-011-0946-8_42
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-4408-0
Online ISBN: 978-94-011-0946-8
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