Gravitational clustering of galaxies - Comparison between thermodynamic theory and n-body simulations

Details Gravitational clustering of galaxies - Comparison between thermodynamic theory and n-body simulations Gravitational clustering of galaxies - Comparison between thermodynamic theory and n-body simulations

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...331...45i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 1, 1988, p. 45-63. Research supported by Kyoto University, Inamor

Other

44

Astronomical Models, Galactic Clusters, Many Body Problem, Thermodynamic Equilibrium, Asymptotic Methods, Gravitational Collapse, Hydrodynamic Equations, Velocity Distribution

Scientific paper

N-body simulations show that homogeneous gravitational clustering in an expanding universe evolves slowly through a series of quasi-equilibrium states. This fundamental result, in agreement with previous theory, greatly simplifies the description of clustering, especially in the nonlinear regime. Detailed comparisons of the thermodynamic theory with these new N-body experiments show that, for a given initial distribution, the rate and degree of relaxation toward the thermodynamic distribution are greater for larger values of Omega(0). This rate is modified if there is a large initial peculiar velocity dispersion, or a very small softening parameter, but the asymptotic state does not depend significantly on either of these. Initially cold or warm Omega(0) = 1 models with a Poisson distribution relax very quickly to the thermodynamic form. They come into agreement with the theory after the universe expands by a factor of about 1.5. The three-dimensional volume and the two-dimensional projected distribution functions also agree well with each other.

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