Cluster infall with friction

Details Cluster infall with friction Cluster infall with friction

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...369...13c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 369, March 1, 1991, p. 13-19. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

42

Dark Matter, Galactic Clusters, Galactic Evolution, Interacting Galaxies, Density Distribution, Dynamic Characteristics, Many Body Problem

Scientific paper

A completely dissipationless N-body numerical simulation of the formation of a small galactic cluster is reported. Galaxy tracers are identified as the high-density regions of the galaxy-scale halos present prior to cluster formation. The largest cluster in the simulation is measured and found to have b(vr) of about 0.8 in the radial velocity dispersion with a galaxy population in better accord with cluster observations than the dark matter distribution. Comparison of the energy history of infalling material shows that the dense cores of dark halos, where galaxies are located, lose energy approximately as expected for dynamical friction terminated by tidal disruption.

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