Interaction of HVCs with the Outskirts of Galactic Disks: Turbulence

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dc.creatorSantillan, A.
dc.creatorSanchez-Salcedo, F. J.
dc.creatorKim, J.
dc.creatorFranco, J.
dc.creatorHernandez-Cervantes, L.
dc.date2009-05-01
dc.date.accessioned2026-07-07T13:11:02Z
dc.date.available2026-07-07T13:11:02Z
dc.descriptionThere exist many physical processes that may contribute to the driving of turbulence in galactic disks. Some of them could drive turbulence even in the absence of star formation. For example, hydrodynamic (HD) or magnetohydrodynamic (MHD) instabilities, frequent mergers of small satellite clumps, ram pressure, or infalling gas clouds. In this work we present numerical simulations to study the interaction of compact high velocity clouds (CHVC) with the outskirts of magnetized gaseous disks. With our numerical simulations we show that the rain of small HVCs onto the disk is a potential source of random motions in the outer parts of HI disks.
dc.description4 pages, 3 figures, Proceedings of "The Role of Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?" (Ed. M. de Avillez), in Espinho, Portugal, 18-22 August 2008
dc.identifierhttps://arxiv.org/abs/0905.0134
dc.identifierhttp://arxiv.org/abs/0905.0134
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/229167
dc.subjectAstrophysics of Galaxies
dc.titleInteraction of HVCs with the Outskirts of Galactic Disks: Turbulence
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