Shocks of High Velocity Clouds and the Galactic Disk: 3D Numerical Simulations

Details Shocks of High Velocity Clouds and the Galactic Disk: 3D Numerical Simulations Shocks of High Velocity Clouds and the Galactic Disk: 3D Numerical Simulations

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.233..181h&link_type=abstract

Astrophysics and Space Science, Volume 233, Issue 1-2, pp. 181-184

Astronomy and Astrophysics

Astrophysics

Ism, Galactic Structure, Hydrodynamics, Shocks

Scientific paper

The ISM shock waves due to the collisions of a high velocity cloud (HVC) and the galactic disk can generate turbulence and star formation processes. As a particular feature, a fraction of gas is ejected out of the disk, and this could be the origin of some molecular complexes like the Chamaeleon andrho Ophiuchi clouds. One can observe some hydrodynamical phases during the shock, when the cloud presents a coalescence stage, followed by re-expansion and deep disk penetration. We present results of evolving shocks done by 3D hydrodynamical simulations of a falling high velocity cloud on the galactic disk with conditions more realistic than preceding studies, with equations which include molecular cooling.

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