Primordial magnetic fields and modified recombination histories

TL;DR

This paper develops a linearized model to compute how primordial magnetic fields influence the recombination history of the universe, addressing computational challenges and providing a framework for future studies on small-scale baryon clumping effects.

Contribution

It introduces a self-consistent, linearized method to calculate modified recombination histories caused by primordial magnetic fields with red-tilted spectra.

Findings

Clumping factors are too small to resolve cosmological tensions.

The framework can be applied to various PMF spectra.

Provides a theoretical basis for future detailed recombination modeling.

Abstract

Recent cosmological data and astrophysical observations, such as the Hubble tension and the increasing preference from galaxy surveys for dynamical dark energy, have begun to challenge the standard $\Lambda$-cold dark matter cosmological model. Primordial magnetic fields (PMFs) offer a mechanism to alleviate these tensions within the framework of the standard model. These fields source excess small-scale baryon clumping, which can speed up recombination and shrink the comoving sound horizon at the surface of last scattering. Computing the modified recombination history requires coupling the radiative transport of Lyman-$\alpha$ photons to compressible magnetohydronamic simulations. Since doing so is generically computationally intractable, we have developed a linearized treatment which self-consistently computes the modified recombination history in the presence of PMF induced baryon clumping for fields with red-tilted spectra. The clumping factors we find are too small to alleviate outstanding cosmological tensions, but our general framework can be applied to other PMF spectra, and provides a significant theoretical step towards a complete account of recombination in the presence of small-scale baryon clumping.