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Interaction of HVCs with the Outskirts of Galactic Disks: Turbulence

Published online by Cambridge University Press:  17 September 2012

A. Santillán ,
F.J. Sánchez–Salcedo ,
J. Kim ,
J. Franco  and
L. Hernández–Cervantes
A. Santillán
Affiliation:
Dirección General de Servicios de Cómputo Académico, UNAM, 04510, Mexico City, Mexico
F.J. Sánchez–Salcedo
Affiliation:
Instituto de Astronomía, UNAM, 04510 Mexico City, Mexico
J. Kim
Affiliation:
Korea Astronomy Observatory, 61–1, Hwaam–Dong, Yusong–Ku, Taejon 305–348, Korea
J. Franco
Affiliation:
Instituto de Astronomía, UNAM, 04510 Mexico City, Mexico
L. Hernández–Cervantes
Affiliation:
Instituto de Astronomía, UNAM, 04510 Mexico City, Mexico
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Abstract

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.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 56: The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall? , 2012 , pp. 343 - 346
Copyright
© EAS, EDP Sciences, 2012

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