Evolution of perturbations in Friedmann models of the universe

Details Evolution of perturbations in Friedmann models of the universe Evolution of perturbations in Friedmann models of the universe

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980afz....16..769s&link_type=abstract

(Astrofizika, vol. 16, Oct.-Dec. 1980, p. 769-779.) Astrophysics, vol. 16, no. 4, Apr. 1981, p. 439-445. Translation.

Astronomy and Astrophysics

Astrophysics

28

Astronomical Models, Cosmology, Gravitation Theory, Perturbation Theory, Universe, Collisionless Plasmas, Density Distribution, Hubble Constant, Space-Time Functions, Specific Heat, Vlasov Equations

Scientific paper

Equations describing the evolution of perturbations of arbitrary magnitude are obtained in the framework of Friedmann cosmological models. It is assumed that the scale of the perturbations is many times less than the distance to the horizon and that the amplitude never attains relativistic values, so that gravitation can be described in the Newtonian approximation. An important feature of the obtained equations is the fact that they are independent of the Hubble constant and ratio of contemporary matter density to that required to close the universe of the cosmological model. Thus, the question of similarity of evolution of perturbations in models with different critical density ratios is solved. The perturbations evolve in three different regimes depending on the type of cosmological model (open, critical, or closed), so that the behavior of the perturbations is similar only within one type of model. However, the transition to a model with a definite critical density ratio for a fixed type of cosmological model is achieved simply by a scale transformation.

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