Magnetic Fields in the Formation of the First Stars. I. Theory vs. Simulation

TL;DR

This paper explores the theoretical origin and simulation of magnetic fields in primordial star formation, highlighting their amplification, effects, and the limitations of current numerical methods.

Contribution

It provides a theoretical framework for magnetic field amplification in early star formation and compares it with simulation results, addressing numerical limitations.

Findings

Magnetic fields of ~10^-16 G are generated and amplified during primordial star formation.

Simulations underestimate magnetic effects due to numerical viscosity and resistivity.

Predicted magnetic flux ratios are comparable to modern star formation.

Abstract

While magnetic fields are important in contemporary star formation, their role in primordial star formation is unknown. Magnetic fields of order 10^-16 G are produced by the Biermann battery due to the curved shocks and turbulence associated with the infall of gas into the dark matter minihalos that are the sites of formation of the first stars. These fields are rapidly amplified by a small-scale dynamo until they saturate at or near equipartition with the turbulence in the central region of the gas. Analytic results are given for the outcome of the dynamo, including the effect of compression in the collapsing gas. The mass-to-flux ratio in this gas is 2-3 times the critical value, comparable to that in contemporary star formation. Predictions of the outcomes of simulations using smooth particle hydrodynamics (SPH) and grid-based adaptive mesh refinement (AMR) are given. Because the numerical viscosity and resistivity for the standard resolution of 64 cells per Jeans length are several orders of magnitude greater than the physical values, dynamically significant magnetic fields affect a much smaller fraction of the mass in simulations than in reality. An appendix gives an analytic treatment of free-fall collapse, including that in a constant density background. Another appendix presents a new method of estimating the numerical viscosity; results are given for both SPH and grid-based codes.