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Formation of shells in major mergersNumerical simulations are used to study the fate of disks in mergers between equal-mass galaxies. Contrary to popular belief, mergers between equal-mass galaxies can form shells, loops, and ripples. Material that was originally in the outer disk of the premerger spirals falls into the remnant late in the merger event, long after the inner region of the remnant has relaxed. Thus, its evolution is similar to that of an accreted dwarf satellite that forms shells through 'phase wrapping'. However, the mechanism described in this letter avoids a number of difficulties with the accretion model; specifically, it can explain the observed correlation between properties of the host galaxies and shell alignments and luminosities. In view of this, we argue that many shell systems may have originated through 'major' mergers of comparable-mass galaxies rather than via 'minor' mergers or accretions. In particular, the shell elliptical NGC 3923 appears to be a good candidate for shell formation by a major merger.
Document ID
19930031018
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Hernquist, Lars
(California Univ. Santa Cruz, United States)
Spergel, David N.
(Princeton Univ. Observatory, NJ, United States)
Date Acquired
August 15, 2013
Publication Date
November 10, 1992
Publication Information
Publication: Astrophysical Journal, Part 2 - Letters
Volume: 399
Issue: 2
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
93A15015
Funding Number(s)
CONTRACT_GRANT: NSF AST-88-58145
CONTRACT_GRANT: NSF AST-90-18526
CONTRACT_GRANT: NAGW-2448
CONTRACT_GRANT: NAGW-2422
CONTRACT_GRANT: NSF AST-91-17388
Distribution Limits
Public
Copyright
Other

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