English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Magnetizing the circumgalactic medium of disc galaxies

MPS-Authors
/persons/resource/persons4732

Pakmor,  Rüdiger
Stellar Astrophysics, MPI for Astrophysics, Max Planck Society;

/persons/resource/persons241099

van de Voort,  Freeke
Galaxy Formation, Cosmology, MPI for Astrophysics, Max Planck Society;

/persons/resource/persons222724

Bieri,  Rebekka
Galaxy Formation, MPI for Astrophysics, Max Planck Society;

/persons/resource/persons232866

Grand,  Robert J. J.
Galaxy Formation, Cosmology, MPI for Astrophysics, Max Planck Society;

/persons/resource/persons4606

Springel,  Volker
Computational Structure Formation, MPI for Astrophysics, Max Planck Society;

External Resource
No external resources are shared
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Pakmor, R., van de Voort, F., Bieri, R., Gómez, J. M., Grand, R. J. J., Guillet, T., et al. (2020). Magnetizing the circumgalactic medium of disc galaxies. Monthly Notices of the Royal Astronomical Society, 498(3), 3125-3137. doi:10.1093/mnras/staa2530.


Cite as: http://hdl.handle.net/21.11116/0000-0007-D6F1-7
Abstract
The circumgalactic medium (CGM) is one of the frontiers of galaxy formation and intimately connected to the galaxy via accretion of gas on to the galaxy and gaseous outflows from the galaxy. Here, we analyse the magnetic field in the CGM of the Milky Way-like galaxies simulated as part of the auriga project that constitutes a set of high-resolution cosmological magnetohydrodynamical zoom simulations. We show that before z = 1 the CGM becomes magnetized via galactic outflows that transport magnetized gas from the disc into the halo. At this time, the magnetization of the CGM closely follows its metal enrichment. We then show that at low redshift an in situ turbulent dynamo that operates on a time-scale of Gigayears further amplifies the magnetic field in the CGM and saturates before z = 0. The magnetic field strength reaches a typical value of 0.1μG at the virial radius at z = 0 and becomes mostly uniform within the virial radius. Its Faraday rotation signal is in excellent agreement with recent observations. For most of its evolution, the magnetic field in the CGM is an unordered small-scale field. Only strong coherent outflows at low redshift are able to order the magnetic field in parts of the CGM that are directly displaced by these outflows.