Magnetic heating across the cosmological recombination era: Results from 3D MHD simulations

TL;DR

This paper uses 3D MHD simulations to explore how primordial magnetic fields evolve and dissipate energy across the recombination era, affecting baryonic heating and turbulence in the early Universe.

Contribution

It introduces detailed numerical modeling of magnetic energy decay and baryon heating during recombination, revealing new transition and decay regimes with delayed turbulence onset.

Findings

No significant heating before recombination

Magnetic energy decays into baryon kinetic energy during transition

Turbulent decay persists after recombination, affecting cosmic microwave background constraints

Abstract

The origin of cosmic magnetic fields is an unsolved problem and magnetogenesis could have occurred in the early Universe. We study the evolution of such primordial magnetic fields across the cosmological recombination epoch via 3D magnetohydrodynamic numerical simulations. We compute the effective or net heating rate of baryons due to decaying magnetic fields and its dependence on the magnetic field strength and spectral index. In the drag-dominated regime ($z \gtrsim 1500$), prior to recombination, we find no real heating is produced. Our simulations allow us to smoothly trace a new transition regime ($600 \lesssim z \lesssim 1500$), where magnetic energy decays, at first, into the kinetic energy of baryons. A turbulent velocity field is built up until it saturates, as the net heating rate rises from a low value at recombination to its peak towards the end of the transition regime. This is followed by a turbulent decay regime ($z \lesssim 600$) where magnetic energy dissipates via turbulent decay of both magnetic and velocity fields while net heating remains appreciable and declines slowly. Both the peak of the net heating rate and the onset of turbulent decay are delayed significantly beyond recombination, by up to 0.5 Myr (until $z\simeq 600-700$), for scale-invariant magnetic fields. We provide analytic approximations and present numerical results for a range of field strengths and spectral indices, illustrating the redshift-dependence of dissipation and net heating rates. These can be used to study cosmic microwave background constraints on primordial magnetic fields.