Gravitational clustering of galaxies: Comparison of thermodynamic theory and N-body simulations. II - The effects of different mass components

Details Gravitational clustering of galaxies: Comparison of thermodynamic theory and N-body simulations. II - The effects of different mass components Gravitational clustering of galaxies: Comparison of thermodynamic theory and N-body simulations. II - The effects of different mass components

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..315i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 20, 1990, p. 315-331. Research supported by the Itoh Science Foun

Statistics

Computation

20

Computational Astrophysics, Galactic Clusters, Gravitational Effects, Many Body Problem, Thermodynamics, Distribution Functions, Galactic Evolution, Galactic Mass, Identifying, Mass Spectra, Spatial Distribution

Scientific paper

The thermodynamic theory of gravitational galaxy clustering gives a good description of the galaxy distribution for both N-body simulations and observations. This theory and the previous N-body simulations, however, assume that all the galaxies have the same mass m. This paper investigates the effects of mass spectra, using new N-body simulations with two mass components (m1 and m2), and it is found that the thermodynamic theory is applicable to two-component systems as long as the mass ratio of two components is in the approximate range of m1:m2 = 1:1-1:10. The analyses show that the massive galaxies provide nuclei for clusters and speed up clustering in early stages, but these individual effects disappear and collective interactions dominate in late stages. The number of massive galaxies which are contained in clusters tends to increase as the mass ratio becomes larger. The quantitative role that massive galaxies play in seeding clusters is describes.

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