Mathematics – Probability
Scientific paper
Jul 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.245..255h&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 245, July 15, 1990, p. 255-267. Research supported by C
Mathematics
Probability
4
Galactic Evolution, Galactic Mass, Galactic Structure, Gravitational Effects, Molecular Clouds, Mass Distribution, Velocity Distribution
Scientific paper
This paper introduces a new approach to the calculation of the galactic mass multiplicity function based on the probability of correlated velocity structures existing on a given spatial scale. The correlations are supposed to have developed during a protogalactic era of virialized structures, before which time the density evolution had already become nonlinear. The density index is determined empirically, although it may eventually be related to a spectrum of initial fluctuations. The subsequent nonlinear dynamics is dealt with explicitly using a continuum model with tidal interactions simulated by an effective shear viscosity. The predictions for the (unnormalized) mass function and for the large-scale velocity correlations between galaxies are deduced relatively directly from the 'cosmic von Karman-Howarth' equation implicit in the basic model. The predictions are in good agreement with existing data.
Henriksen Richard N.
Lachièze-Rey Marc
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