We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

Magnetic field formation in the Milky Way like disc galaxies of the Auriga project.

Pakmor, R. and Gómez, F. A. and Grand, R. J. J. and Marinacci, F. and Simpson, C. M. and Springel, V. and Campbell, D. J. R. and Frenk, C. S. and Guillet, T. and Pfrommer, C. and White, S. D. M. (2017) 'Magnetic field formation in the Milky Way like disc galaxies of the Auriga project.', Monthly notices of the Royal Astronomical Society., 469 (3). pp. 3185-3199.


The magnetic fields observed in the Milky Way and nearby galaxies appear to be in equipartition with the turbulent, thermal and cosmic ray energy densities, and hence are expected to be dynamically important. However, the origin of these strong magnetic fields is still unclear, and most previous attempts to simulate galaxy formation from cosmological initial conditions have ignored them altogether. Here, we analyse the magnetic fields predicted by the simulations of the Auriga Project, a set of 30 high-resolution cosmological zoom simulations of Milky Way like galaxies, carried out with a moving-mesh magnetohydrodynamics code and a detailed galaxy formation physics model. We find that the magnetic fields grow exponentially at early times owing to a small-scale dynamo with an e-folding time of roughly 100 Myr in the centre of haloes until saturation occurs around z = 2–3, when the magnetic energy density reaches about 10 per cent of the turbulent energy density with a typical strength of 10--50μG 10--50μG . In the galactic centres, the ratio between magnetic and turbulent energies remains nearly constant until z = 0. At larger radii, differential rotation in the discs leads to linear amplification that typically saturates around z = 0.5–0. The final radial and vertical variations of the magnetic field strength can be well described by two joint exponential profiles, and are in good agreement with observational constraints. Overall, the magnetic fields have only little effect on the global evolution of the galaxies as it takes too long to reach equipartition. We also demonstrate that our results are well converged with numerical resolution.

Item Type:Article
Full text:(VoR) Version of Record
First Live Deposit - 18 July 2017
Download PDF
Publisher Web site:
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
Record Created:18 Jul 2017 12:13
Last Modified:31 Aug 2017 14:59

Social bookmarking: del.icio.usConnoteaBibSonomyCiteULikeFacebookTwitterExport: EndNote, Zotero | BibTex
Look up in GoogleScholar | Find in a UK Library