2001/12/04 by Hongsheng Zhao, HongSheng Zhao, Zhao, HongSheng
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0112094
8 pages with 3 PS figs, minor correction, to be published in the "Omega Centauri: a Unique Window into Astrophysics" (Cambridge, Aug. 2001), ASP Conf. Ser. edited by F. van Leeuwen, G. Piotto,and J. Hughes
arxiv created 2001/12/06 · arxiv updated 2009/12/01
We simulate the result of orbital decay for a dwarf satellite galaxy in a disk galaxy potential. The peeling-off of the satellite by the strong tidal field within the disk of the host galaxy quickly reduces the satellite's mass, and drastically slows down the decaying of the orbit. The result is generally a cluster on a large halo orbit, like the M54 cluster of the Sagittarius galaxy in the Milky Way and the massive G1 cluster in outer halo of M31. It is generally challenging for this mechanism to deliver globular cluster-mass objects to the observed very close-in orbit of Omega Cen unless the dwarf galaxy was born within a few scale lengths of the Galactic disk.