Evolution of perturbations in expanding universe

Details Evolution of perturbations in expanding universe Evolution of perturbations in expanding universe

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987rpsct..11...54k&link_type=abstract

In its JPRS Report: Science and Technology. USSR: Physics and Mathematics p 54 (SEE N88-14727 06-70) Transl. into ENGLISH from P

Mathematics

Cosmology, Evolution (Development), Perturbation, Universe, Differential Equations, Einstein Equations

Scientific paper

The behavior of perturbations during evolution of the universe, particularly in its expanding stage, is analyzed on the basis of the gravitation theory with total action and inclusion of higher order derivatives. Using the metrics of the flat homogeneous and isotropic cosmological model with small scalar perturbations for the relativistic gauge potential, a system of two equations of perturbations differential with respect to conformal time is derived from the system of corresponding two Einstein equations. They are then reduced to a single second-order differential equation in a new variable. This equation is solved asymptotically. Considering that the large class of solution to the Einstein equations for the quiescent phonon model includes the asymptotic quasi-deSitter mode of evolution, the solution is extended to the subsequent scalar stage. Perturbations, conformally plane in the quasi-deSitter stage, are found to become conformally Newtonian upon transition to the scalar stage and to build up to the galactic scale while shifting from the short-wave mode to the long-wave mode. The amplification factor 3.6H squared/M squared is constrained by H 5 times 10 to the 13th and M 10 to the 13th GeV.

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