Mapping the Galactic Magnetic Field Orientation and Strength in Three Dimensions
Yue Hu, Alex Lazarian

TL;DR
This paper presents a novel 3D mapping of the Galactic Magnetic Field's orientation and strength using advanced techniques and H I emission data, revealing sub-Alfvénic and subsonic gas properties in the Milky Way.
Contribution
It introduces a new method combining MM2, VGT, and H I data to map the GMF in three dimensions, including magnetic field strength and turbulence parameters.
Findings
Magnetic field strength varies from ~0.5 to 2.5 μG.
The gas is predominantly sub-Alfvénic and subsonic.
Magnetic field strength decreases towards the Galaxy's outskirts.
Abstract
The mapping of the Galactic Magnetic Field (GMF) in three dimensions is essential to comprehend various astrophysical processes that occur within the Milky Way. This study endeavors to map the GMF by utilizing the latest MM2 technique, the Velocity Gradient Technique (VGT), the Column Density Variance Approach, and the GALFA-H I survey of Neutral Hydrogen (H I) emission. The MM2 and VGT methods rely on an advanced understanding of magnetohydrodynamics turbulence to determine the magnetic field strength and orientation respectively. The H I emission data, combined with the Galactic rotational curve, gives us the distribution of H I gas throughout the Milky Way. By combining these two techniques, we map the GMF orientation and strength, as well as the Alfv\'en Mach number in 3D for a low galactic latitude () region close to the Perseus Arm. The analysis of column…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
Taxonomy
TopicsStellar, planetary, and galactic studies · Astrophysics and Star Formation Studies · Solar and Space Plasma Dynamics
