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

• Verfasst von: Pakmor, Rüdiger [VerfasserIn]
• Verfasst von: Grand, Robert J. J. [VerfasserIn]
• Verfasst von: Springel, Volker [VerfasserIn]
• Verfasst von: Guillet, Thomas [VerfasserIn]
• Verfasst von: Pfrommer, Christoph [VerfasserIn]
• Titel: Magnetic field formation in the Milky Way like disc galaxies of the Auriga project
• Verf.angabe: Rüdiger Pakmor, Facundo A. Gómez, Robert J.J. Grand, Federico Marinacci, Christine M. Simpson, Volker Springel, David J.R. Campbell, Carlos S. Frenk, Thomas Guillet, Christoph Pfrommer and Simon D.M. White
• E-Jahr: 2017
• Jahr: 04 May 2017
• Umfang: 15 S.
• Fussnoten: Gesehen am 19.10.2017
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2017
• Band/Heft Quelle: 469(2017), 3, Seite 3185-3199
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stx1074
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1564561917

Abstract

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 $$10\text{--}50\,\rm {\mu G}$$. 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.