Galaxy clustering and thermodynamics - Quasi-static evolution of b(t)

Details Galaxy clustering and thermodynamics - Quasi-static evolution of b(t) Galaxy clustering and thermodynamics - Quasi-static evolution of b(t)

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...304...11s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 304, May 1, 1986, p. 11-14.

Astronomy and Astrophysics

Astrophysics

16

Cosmology, Galactic Clusters, Gravitation, Kinetic Energy, Thermodynamics, Asymptotic Properties, Bbgky Hierarchy, Ratios

Scientific paper

Combining the cosmic energy equation with the BBGKY clustering hierarchy gives a simple evolution equation for b(t), the ratio of gravitational correlation energy to kinetic energy in the expanding universe. It applies most accurately to the case of an initially unclustered distribution. The asymptotic value of this ratio for nonlinear clustering is (2α+1)/(2α+2), where the cosmic scale length R(t)∝tα. This agrees with the observed value of b = 0.7±0.05 for the distribution of galaxies in our universe for α near the Einstein-de Sitter value of 2/3.

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