Development of cosmological perturbations in a large-scale inhomogeneous background

Details Development of cosmological perturbations in a large-scale inhomogeneous background Development of cosmological perturbations in a large-scale inhomogeneous background

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993azh....70..657n&link_type=abstract

Astronomicheskij Zhurnal, vol. 70, p. 657

Astronomy and Astrophysics

Astronomy

2

Gravitational Collapse, Density Distribution, Nonuniform Plasmas, Linear Evolution Equations, Perturbation Theory, Galactic Evolution

Scientific paper

Solutions of evolution equations for linear perturbations in a spherically symmetric inhomogeneous background with an arbitrary density distribution are obtained. It is shown that growth speed of density perturbations increases as compared to that with perturbations in a critical background. At the turn-around moment for a homogeneous background with Omega greater than 1, the amplitude of perturbations is three times as great as that in the flat Friedman background. In the galaxy formation problem, this effect is essential in models with density fluctuation spectra which contain greater power at scales of clusters of galaxy-size and larger. This effect may be responsible for the fragmentation of a large-scale perturbations into small-scale objects.

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