The Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows

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dc.creatorHeitsch, F.
dc.creatorSlyz, A. D.
dc.creatorDevriendt, J. E. G.
dc.creatorHartmann, L. W.
dc.creatorBurkert, A.
dc.date2006-05-17
dc.date.accessioned2026-07-07T10:39:02Z
dc.date.available2026-07-07T10:39:02Z
dc.descriptionMolecular Cloud Complexes (MCCs) are highly structured and ``turbulent''. Observational evidence suggests that MCCs are dynamically dominated systems, rather than quasi-equilibrium entities. The observed structure is more likely a consequence of the formation process rather than something that is imprinted after the formation of the MCC. Converging flows provide a natural mechanism to generate MCC structure. We present a detailed numerical analysis of this scenario. Our study addresses the evolution of a MCC from its birth in colliding atomic hydrogen flows up until the point when H$_2$ may begin to form. A combination of dynamical and thermal instabilities breaks up coherent flows efficiently, seeding the small-scale non-linear density perturbations necessary for local gravitational collapse and thus allowing (close to) instantaneous star formation. Many observed properties of MCCs come as a natural consequence of this formation scenario. Since converging flows are omnipresent in the ISM, we discuss the general applicability of this mechanism, from local star formation regions to galaxy mergers.
dc.description15 pages, 20 figures, accepted by ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0605435
dc.identifierhttp://arxiv.org/abs/astro-ph/0605435
dc.identifierAstrophys.J.648:1052-1065,2006
dc.identifierdoi:10.1086/505931
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180888
dc.subjectAstrophysics
dc.titleThe Birth of Molecular Clouds: Formation of Atomic Precursors in Colliding Flows
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