A precise numerical estimation of the magnetic field generated around recombination

TL;DR

This paper provides a detailed numerical estimation of the magnetic field generated during recombination, revealing it to be extremely weak and highlighting limitations of current computational methods for small-scale predictions.

Contribution

The study improves the accuracy of magnetic field spectrum estimation around recombination using high-resolution second-order Boltzmann code simulations.

Findings

Magnetic field generated up to redshift ~10.

Field strength around 2×10^{-29} G on Mpc scales.

Previous studies lacked sufficient angular resolution.

Abstract

We investigate the generation of magnetic fields from non-linear effects around recombination. As tight-coupling is gradually lost when approaching $z\simeq 1100$, the velocity difference between photons and baryons starts to increase, leading to an increasing Compton drag of the photons on the electrons. The protons are then forced to follow the electrons due to the electric field created by the charge displacement; the same field, following Maxwell's laws, eventually induces a magnetic field on cosmological scales. Since scalar perturbations do not generate any magnetic field as they are curl-free, one has to resort to second-order perturbation theory to compute the magnetic field generated by this effect. We reinvestigate this problem numerically using the powerful second-order Boltzmann code SONG. We show that: i) all previous studies do not have a high enough angular resolution to reach a precise and consistent estimation of the magnetic field spectrum; ii) the magnetic field is generated up to $z\simeq 10$; iii) it is in practice impossible to compute the magnetic field with a Boltzmann code for scales smaller than $1\,{\rm Mpc}$. Finally we confirm that for scales of a few ${\rm Mpc}$, this magnetic field is of order $2\times 10^{-29}{\rm G}$, many orders of magnitude smaller than what is currently observed on intergalactic scales.