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Encounters of spherical galaxies. I - Galaxy models with one stellar population. II - Galaxy models with two stellar populationsClose encounters between two spherical galaxies of equal size and consisting of only one stellar population are calculated using models of elliptical galaxies constructed according to King's (1966) method. The mass loss and the change in internal energy are computed under the assumption that the stars do not change their velocity or density distributions during the encounters. The results for a specific case are compared with the calculations of Gallagher and Ostriker (1972), who employed the observed brightness distribution and the derived density distribution of the E1 galaxy NGC 3379. For models with one stellar population, the results suggest that the radius of a galactic halo would have to be at least 200 kpc for appreciable mass loss to occur over the history of a galaxy in a rich cluster. The calculations are then extended to include a halo population characterized by a high central velocity dispersion. In this case, it is found that the halo population of sufficiently large galaxies can be dispersed without appreciably affecting the main population. It is suggested that the missing mass of many clusters of galaxies may be located in an intergalactic sea of faint stars making up an envelope for the centrally located gE galaxies.
Document ID
19760047873
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Biermann, P.
(Bonn, Universitaet Bonn, Germany)
Silk, J.
(Bonn Univ. Germany)
Date Acquired
August 8, 2013
Publication Date
April 1, 1976
Publication Information
Publication: Astronomy and Astrophysics
Volume: 48
Issue: 2, Ap
Subject Category
Astrophysics
Accession Number
76A30839
Funding Number(s)
CONTRACT_GRANT: DFG-SFB-131
CONTRACT_GRANT: DFG-BI-191/2
CONTRACT_GRANT: NGR-05-003-578
CONTRACT_GRANT: DFG-BI-191/1
Distribution Limits
Public
Copyright
Other

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