Formation of gas disks in merging galaxies

Details Formation of gas disks in merging galaxies Formation of gas disks in merging galaxies

2002-01-15

arxiv.org/abs/astro-ph/0201250v1

Mon.Not.Roy.Astron.Soc. 333 (2002) 481

Astronomy and Astrophysics

Astrophysics

Submitted to MNRAS. 15 pages, 12 B&W figures, 1 color figure. See http://www.ifa.hawaii.edu/~barnes/fogdimg.html for versions

Scientific paper

10.1046/j.1365-8711.2002.05335.x

Observations indicate that much of the interstellar gas in merging galaxies may settle into extended gaseous disks. Here, I present simulations of disk formation in mergers of gas-rich galaxies. Up to half of the total gas settles into embedded disks; the most massive instances result from encounters in which both galaxies are inclined to the orbital plane. These disks are often warped, many have rather complex kinematics, and roughly a quarter have counter-rotating or otherwise decoupled central components. Disks typically grow from the inside out; infall from tidal tails may continue disk formation over long periods of time.

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