Growth rate of matter perturbations as a probe of large-scale magnetism

TL;DR

This paper investigates how large-scale magnetic fields influence the growth rate of matter perturbations in cosmological models, providing analytical and numerical insights to enhance understanding of structure formation and dark energy.

Contribution

It derives an analytical expression for the growth rate in magnetized environments and explores the effects of relativistic corrections and plasma inhomogeneities.

Findings

Magnetic fields affect matter perturbation growth rates.

Analytical formula applicable when dark energy does not cluster.

Magnetic effects can help distinguish cosmological models.

Abstract

The growth rate of matter perturbations is computed in a magnetized environment for the LambdaCDM and wCDM paradigms. It is argued that the baryons do not necessarily follow into the dark matter potential wells after they are released from the drag of the photons. The baryonic evolution equations inherit a forcing term whose explicit form depends on the plasma description and can be deduced, for instance, in the resistive magnetohydrodynamical approximation. After deriving an analytical expression for the growth rate applicable when dark energy does not cluster, the effects of relativistic corrections and of the inhomogeneities associated with the other species of the plasma are taken into account numerically. The spectral amplitudes and slopes of the stochastic magnetic background are selected to avoid appreciable distortions in the measured temperature and polarization anisotropies of the Cosmic Microwave Background. The growth of structures in the current paradigms of structure formation represents a complementary probe of large-scale magnetism in the same way as the shape of the growth factor and the associated indices can be used, in the conventional lore, to discriminate between competing scenarios of dark energy or even to distinguish different models of gravity.