English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/74996
Share/Impact:
Statistics
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL
Exportar a otros formatos:
Title

Formation of kinematic subsystems in stellar spiral-spiral mergers

AuthorsBalcells, Marc; González-García, A. César
Keywordsgalaxies: abundances
galaxies: elliptical and lenticular, cD
galaxies: interactions
galaxies: kinematics and dynamics
galaxies: peculiar
Incipit
Institute of Heritage Sciences
Instituto de Ciencias del Patrimonio
Issue Date1-Oct-1998
PublisherInstitute of Physics Publishing
CitationThe Astrophysical Journal, 505 (2): L109-L112. Bristol
Abstract[EN]We show that kinematically peculiar cores may be generated in stellar spiral-spiral mergers. Kinematic segregation appears as the central bulges transport orbital angular momentum inward to the center of the remnant, while the outer parts keep the spin signature of the precursor disks. The peculiar core is composed mostly of bulge material, and its size best matches that of observed peculiar cores for mergers with unequal galaxy masses (~2:1). Population decoupling is predicted by the rapid radial decrease of the bulge fraction in the remnant. In this scenario, a starburst may pump up the remnant metallicity, but otherwise the high metallicity of the kinematically decoupled core is built on the high metal content of the inner bulges rather than on a high selfenrichment of a population built from scratch out of the precursors’ gas. Mergers with galaxy mass ratios 3:1 and above generate disk galaxies with counterrotating bulges.
Publisher version (URL)http://iopscience.iop.org/1538-4357/505/2/L109
URIhttp://hdl.handle.net/10261/74996
DOI10.1086/311617
ISSN0004-637X
E-ISSN1538-4357
Appears in Collections:(INCIPIT) Artículos
Show full item record
Review this work
 

Related articles:


WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.