  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.
