Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....48..287b&link_type=abstract
Astronomy and Astrophysics, vol. 48, no. 2, Apr. 1976, p. 287-293, 295-299. Deutsche Forschungsgemeinschaft
Astronomy and Astrophysics
Astrophysics
5
Astronomical Models, Elliptical Galaxies, Galactic Clusters, Galactic Evolution, Density Distribution, M Stars, Missing Mass (Astrophysics), Star Distribution, Tables (Data)
Scientific paper
Close 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.
Biermann Peter
Silk Joseph
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