Gravitational instability in the early universe - The growth of cluster-sized density perturbations

Details Gravitational instability in the early universe - The growth of cluster-sized density perturbations Gravitational instability in the early universe - The growth of cluster-sized density perturbations

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..285p&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 1, 1978, p. 285-292. Research supported by the Smithsonian Research Foundatio

Astronomy and Astrophysics

Astrophysics

14

Galactic Clusters, Galactic Evolution, Gravitational Collapse, Space Density, Universe, X Ray Sources, Astronomical Models, Cosmology, Density Distribution, Gravitational Fields, Hubble Diagram

Scientific paper

The growth of density perturbations in the early universe is computed for the case of spherical perturbations with a surrounding 'hole'. The analytical results are applied to the problem of infalling intergalactic material for the case of the Coma cluster, and it is found that the constraint given by Gunn and Gott (1972) on the amount of infallen material is relaxed only slightly. The location of the 'turnaround' radius near clusters is also computed. Although the turnaround radius Rt is insensitive to q0, the fraction of mass within Rt which is not yet virialized varies significantly with q0. It is suggested that the high X-ray luminosity of superclusters is due to the enhanced growth by gravitational instability of individual clusters in a supercluster environment. These individual X-ray clusters are likely to be of sufficient luminosity to explain the supercluster X-ray emission.

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