Models of the Effect of Gaseous Drag on the Accretion of Intergalactic Clouds

Details Models of the Effect of Gaseous Drag on the Accretion of Intergalactic Clouds Models of the Effect of Gaseous Drag on the Accretion of Intergalactic Clouds

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.1509f&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #15.09; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Neutral gas clouds are observed outside the disks of ordinary spiral galaxies like the Milky Way. The high velocity clouds of our own Galaxy, assumed to be within 200 kpc, show evidence of interaction with the gaseous halo. We present models of the orbital decay of such clouds over time for a realistic model of the density and velocity structure of the interstellar Galactic disk and halo. We examine the effects of impact parameter, initial velocity, column density and prograde/retrograde trajectories on when such clouds are accreted. We demonstrate that clouds with higher column density, clouds that are retrograde, and clouds with smaller impact parameters will settle deeper into the center of the gaseous galactic disk. This research was supported by NSF REU Site grant to UW-Madison, AST-0453442.

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