Magnetic fields during high redshift structure formation
Abstract
We explore the amplification of magnetic fields in the high-redshift Universe. For this purpose, we perform high-resolution cosmological simulations following the formation of primordial halos with \sim10^7 M_solar, revealing the presence of turbulent structures and complex morphologies at resolutions of at least 32 cells per Jeans length. Employing a turbulence subgrid-scale model, we quantify the amount of unresolved turbulence and show that the resulting turbulent viscosity has a significant impact on the gas morphology, suppressing the formation of low-mass clumps. We further demonstrate that such turbulence implies the efficient amplification of magnetic fields via the small-scale dynamo. We discuss the properties of the dynamo in the kinematic and non-linear regime, and explore the resulting magnetic field amplification during primordial star formation. We show that field strengths of \sim10^{-5} G can be expected at number densities of \sim5 cm^{-3}.
Cite
@article{arxiv.1211.4356,
title = {Magnetic fields during high redshift structure formation},
author = {Dominik R. G. Schleicher and Muhammad Latif and Jennifer Schober and Wolfram Schmidt and Stefano Bovino and Christoph Federrath and Jens Niemeyer and Robi Banerjee and Ralf S. Klessen},
journal= {arXiv preprint arXiv:1211.4356},
year = {2015}
}
Comments
7 pages, 6 figures, 1 table. Proceedings article for the 2012 Fall Meeting of the Astronomische Gesellschaft (AG 2012) in Hamburg, submitted for the yearbook series "Reviews in Modern Astronomy", volume 25, of the Astronomische Gesellschaft