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A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields

Liu, T, Li, PS, Juvela, M, Kim, K-T, Evans, NJ, Di Francesco, J, Liu, S-Y, Yuan, J, Tatematsu, K, Zhang, Q, Ward-Thompson, D, Fuller, G, Goldsmith, PF, Koch, PM, Sanhueza, P, Ristorcelli, I, Kang, S-J, Chen, H-R, Hirano, N, Wu, Y , Sokolov, V, Lee, CW, White, GJ, Wang, K, Eden, DJ, Li, D, Thompson, M, Pattle, KM, Soam, A, Nasedkin, E, Kim, J, Kim, G, Lai, S-P, Park, G, Qiu, K, Zhang, C-P, Alina, D, Eswaraiah, C, Falgarone, E, Fich, M, Greaves, J, Gu, Q-L, Kwon, W, Li, H-B, Malinen, J, Montier, L, Parsons, H, Qin, S-L, Rawlings, MG, Ren, Z-Y, Tang, M, Tang, Y-W, Toth, LV, Wang, J, Wouterloot, J, Yi, H-W and Zhang, H-W (2018) A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields. Astrophysical Journal, 859 (2). ISSN 0004-637X

A Holistic Perspective on the Dynamics of G035.39-00.33 The Interplay between Gas and Magnetic Fields.pdf - Accepted Version

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Magnetic field plays a crucial role in shaping molecular clouds and regulating star formation, yet the complete information on the magnetic field is not well constrained owing to the limitations in observations. We study the magnetic field in the massive infrared dark cloud G035.39-00.33 from dust continuum polarization observations at 850 μm with SCUBA-2/POL-2 at JCMT for the first time. The magnetic field tends to be perpendicular to the densest part of the main filament (F M), whereas it has a less defined relative orientation in the rest of the structure, where it tends to be parallel to some diffuse regions. A mean plane-of-the-sky magnetic field strength of ~50 μG for F M is obtained using the Davis–Chandrasekhar–Fermi method. Based on 13CO (1–0) line observations, we suggest a formation scenario of F M due to large-scale (~10 pc) cloud–cloud collision. Using additional NH3 line data, we estimate that F M will be gravitationally unstable if it is only supported by thermal pressure and turbulence. The northern part of F M, however, can be stabilized by a modest additional support from the local magnetic field. The middle and southern parts of F M are likely unstable even if the magnetic field support is taken into account. We claim that the clumps in F M may be supported by turbulence and magnetic fields against gravitational collapse. Finally, we identified for the first time a massive (~200 M ⊙), collapsing starless clump candidate, "c8," in G035.39-00.33. The magnetic field surrounding "c8" is likely pinched, hinting at an accretion flow along the filament.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical and Space Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, 0306 Physical Chemistry (incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society; IOP Publishing
Related URLs:
Date Deposited: 09 Oct 2019 09:50
Last Modified: 04 Sep 2021 08:43
DOI or ID number: 10.3847/1538-4357/aac025
URI: https://researchonline.ljmu.ac.uk/id/eprint/11505
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