Zooming in on the circumgalactic medium with GIBLE: the topology and draping of magnetic fields around cold clouds : letter to the editor
We used a cosmological zoom-in simulation of a Milky Way-like galaxy to study and quantify the topology of magnetic field lines around cold gas clouds in the circumgalactic medium (CGM). This simulation is a new addition to Project GIBLE, a suite of cosmological magnetohydrodynamic simulations of ga...
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| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) Editorial |
| Sprache: | Englisch |
| Veröffentlicht: |
April 2024
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| In: |
Astronomy and astrophysics
Year: 2024, Jahrgang: 684, Pages: 1-6 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202348786 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202348786 Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2024/04/aa48786-23/aa48786-23.html 
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| Verfasserangaben: | Rahul Ramesh, Dylan Nelson, Drummond Fielding, and Marcus Brüggen |
MARC
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| 520 | |a We used a cosmological zoom-in simulation of a Milky Way-like galaxy to study and quantify the topology of magnetic field lines around cold gas clouds in the circumgalactic medium (CGM). This simulation is a new addition to Project GIBLE, a suite of cosmological magnetohydrodynamic simulations of galaxy formation with preferential super-Lagrangian refinement in the CGM, reaching an unprecedented CGM gas mass resolution of ∼225 M⊙. To maximize statistics and resolution, we focused on a sample of ∼200 clouds with masses of ∼106 M⊙. The topology of magnetic field lines around clouds is diverse, from threading to draping, and there is large variation in the magnetic curvature (κ) within cloud-background interfaces. We typically find little variation of κ between upstream and downstream cloud faces, implying that strongly draped configurations are rare. In addition, κ correlates strongly with multiple properties of the interface and the ambient background, including cloud overdensity and relative velocity, suggesting that cloud properties impact the topology of interface magnetic fields. | ||
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