The growth of structure in the Szekeres inhomogeneous cosmological models and the matter-dominated era

TL;DR

This paper investigates the growth of large-scale structure in Szekeres inhomogeneous cosmological models, revealing significantly stronger growth rates than standard FLRW models, which could impact dark matter interpretations.

Contribution

It introduces exact non-linear growth equations in Szekeres models and demonstrates their stronger structure growth compared to FLRW and spherical collapse models.

Findings

Growth rate up to 3-5 times stronger than linear FLRW models

Exact non-linear perturbations significantly enhance structure growth

Differences increase over time, highlighting inhomogeneity effects

Abstract

This study belongs to a series devoted to using Szekeres inhomogeneous models to develop a theoretical framework where observations can be investigated with a wider range of possible interpretations. We look here into the growth of large-scale structure in the models. The Szekeres models are exact solutions to Einstein's equations that were originally derived with no symmetries. We use a formulation of the models that is due to Goode and Wainwright, who considered the models as exact perturbations of an FLRW background. Using the Raychaudhuri equation, we write for the two classes of the models, exact growth equations in terms of the under/overdensity and measurable cosmological parameters. The new equations in the overdensity split into two informative parts. The first part, while exact, is identical to the growth equation in the usual linearly perturbed FLRW models, while the second part constitutes exact non-linear perturbations. We integrate numerically the full exact growth rate equations for the flat and curved cases. We find that for the matter-dominated era, the Szekeres growth rate is up to a factor of three to five stronger than the usual linearly perturbed FLRW cases, reflecting the effect of exact Szekeres non-linear perturbations. The growth is also stronger than that of the non-linear spherical collapse model, and the difference between the two increases with time. This highlights the distinction when we use general inhomogeneous models where shear and a tidal gravitational field are present and contribute to the gravitational clustering. Additionally, it is worth observing that the enhancement of the growth found in the Szekeres models during the matter-dominated era could suggest a substitute to the argument that dark matter is needed when using FLRW models to explain the enhanced growth and resulting large-scale structures that we observe today (abridged)