期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 333, 期 3, 页码 481-494出版社
BLACKWELL PUBLISHING LTD
DOI: 10.1046/j.1365-8711.2002.05335.x
关键词
hydrodynamics; stellar dynamics; galaxies : formation; galaxies : interactions; galaxies : kinematics and dynamics; galaxies : structure
Observations indicate that much of the interstellar gas in merging galaxies may settle into extended gaseous discs. Here, I present simulations of disc formation in mergers of gas-rich galaxies. Up to half of the total gas settles into embedded discs; the most massive instances result from encounters in which both galaxies are inclined to the orbital plane. These discs are often warped, many have rather complex kinematics, and roughly a quarter have counter-rotating or otherwise decoupled central components. Discs typically grow from the inside out; infall from tidal tails may continue disc formation over long periods of time.
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