The growth of the density fluctuations in the scale-invariant vacuum theory

Abstract

The growth of the density fluctuations is considered to be an important cosmological test. In the standard model, for a matter dominated universe, the growth of the density perturbations evolves with redshift z like (11+z)s with s=1. This is not fast enough to form galaxies and to account for the observed present-day inhomogeneities. This problem is usually resolved by assuming that at the recombination epoch the baryons settle down in the potential well of the dark matter previously assembled during the radiation era of the universe. This view is challenged in the present paper by using the recently proposed model of a scale-invariant framework for cosmology, the Scale-Invariant Vacuum Theory (Maeder 2017a,2017b,2017c), that enlarges the invariance group subtending the theory of the gravitation. From the continuity equation, the Euler and Poisson equations are written in the scale-invariant framework, the equation governing the growth of density fluctuations δ is obtained. Starting from δ=10−5 at a redshift around 1000, numerical solutions for various density background are obtained. The growth of density fluctuations is much faster than in the standard EdS model. The s values are in the range from 2.7 to 3.9 for Ωm between 0.30 and 0.02. This enables the density fluctuations to enter the nonlinear regime with δ>1 long before the present time, typically at redshifts of about 10, without requiring the presence of dark matter.