Magnetic fields from small-scale primordial perturbations

Abstract

Weak magnetic fields must have existed in the early Universe, as they were sourced by the cross product of electron density and temperature gradients through the Biermann-battery mechanism. In this paper we calculate the magnetic fields generated at cosmic dawn by a variety of small-scale primordial perturbations, carefully computing the evolution of electron density and temperature fluctuations, and consistently accounting for relative velocities between baryons and dark matter. We first compute the magnetic field resulting from standard, nearly scale-invariant primordial adiabatic perturbations, making significant improvements to previous calculations. This "standard" primordial field has a root mean square (rms) of $\sim10^{-15}$ nG at $20\lesssim z \lesssim 100$, with fluctuations on $\sim$ kpc comoving scales, and could serve as the seed of present-day magnetic fields observed in galaxies and galaxy clusters. In addition, we consider early-Universe magnetic fields as a possible probe of non-standard initial conditions of the Universe on small scales $k \sim 1-10^3$ Mpc$^{-1}$. To this end, we compute the maximally-allowed magnetic fields within current upper limits on small-scale adiabatic and isocurvature perturbations. Under the current Cosmic Microwave Background spectral-distortion constraints magnetic fields could be produced with a rms of $\sim 5\times 10^{-11}$ nG at $z = 20$. Uncorrelated small-scale isocurvature perturbations within current Big-Bang Nucleosynthesis bounds could potentially enhance the magnetic field to $\sim 10^{-14}-10^{-10}$ nG at $z = 20$, depending on the specific isocurvature mode considered. While these very weak fields remain well below current observational capabilities, our work points out that magnetic fields could potentially provide an interesting window into the poorly constrained small-scale initial conditions of the Universe.