EAS Publications Series
Volume 56, 2012The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|Page(s)||343 - 346|
|Section||Modelling the Disk-Halo Interaction in Galaxies|
|Published online||17 September 2012|
Miguel A. de Avillez (ed)
EAS Publications Series, 56 (2012) 343–346
Interaction of HVCs with the Outskirts of Galactic Disks: Turbulence
1 Dirección General de Servicios de Cómputo Académico, UNAM, 04510, Mexico City, Mexico
2 Instituto de Astronomía, UNAM, 04510 Mexico City, Mexico
3 Korea Astronomy Observatory, 61–1, Hwaam–Dong, Yusong–Ku, Taejon 305–348, Korea
There 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.
© EAS, EDP Sciences, 2012