2020/12/14 by Kohei Kurahara, Hiroyuki Nakanishi, Yuki Kudoh
Chemistry · Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Chemistry #Galaxies: Formation, Evolution, Phenomena #Galaxy #Magnetic field #Physics #Polarization (electrochemistry) #Spiral galaxy #Stellar, planetary, and galactic studies #Vector field #astro-ph.GA
paper · pdf · doi:10.1093/pasj/psaa116
10 pages, 8 figures and 3 tables. Accepted for publication in PASJ
openalex publication_date 2020/12/14 · arxiv created 2020/12/17 · arxiv updated 2021/01/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We analyzed the data of Stokes I, Q, and U in the C and X bands and investigated the large-scale magnetic field structure of NGC 3627. The polarization intensity and angle in each band were derived using Stokes Q and U maps. The rotation measure was calculated using polarization angle maps. Moreover, the magnetic field strength was calculated by assuming energy equipartition with cosmic ray electrons. The structure of the magnetic field was well aligned with the spiral arms, which were consistent with those in the former studies. We applied the magnetic vector reconstruction method to NGC 3627 to derive a magnetic vector map, which showed that the northern and southern disks were dominant with inward and outward magnetic vectors, respectively. Furthermore, we considered the large-scale structure of the magnetic field in NGC 3627 and observed that the structure is bi-symmetric spiral in nature, and that the number of magnetic field modes is mB = 1 in the outer region of galaxy. In addition, NGC 3627 has a mode of two spiral arms that were clearly visible in an optical image. The ratio of the mode of the spiral arms to that of the magnetic field is 2 : 1. In terms of NGC 3627, the large-scale magnetic field may be generated via the parametric resonance induced by the gravitational potential of the spiral arms.