The evolution of clusters of galaxies. I - Very rich clusters

Details The evolution of clusters of galaxies. I - Very rich clusters The evolution of clusters of galaxies. I - Very rich clusters

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...268...30r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 268, May 1, 1983, p. 30-46. Research supported by the Research Corp.

Physics

100

Celestial Mechanics, Galactic Clusters, Galactic Evolution, Mass Distribution, Monte Carlo Method, Collision Parameters, Elliptical Galaxies, Intergalactic Media, Kinetic Friction, Mass Spectra, Mass To Light Ratios, Relaxation Time, Stochastic Processes, Tides, Virial Theorem

Scientific paper

A multiple one-body Monte Carlo code is used to investigate the evolution of galaxies in a steady cluster potential under the influence of dynamical friction, two-body relaxation, tidal stripping, and galaxy mergers. The basic assumptions, estimated time scales, method and computer program, and effects of uncertainties in galaxy encounter physics are addressed. Numerical experiments in which the mass initially carried by galaxies and the mass function are varied are reported. It is shown that the formation of a very massive cluster galaxy depends critically on the number of galaxies, the initial division of cluster material between galaxies and a smooth intracluster medium, the mass spectrum of the galaxies, and chance. By the end of all simulations, less than half of the mass in the central regions of the cluster is bound to galaxies. It appears possible to produce any of the Bautz-Morgan classes from very similar initial conditions.

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