A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields
Liu,Tie1,2; Li,Pak Shing3; Juvela,Mika4; Kim,Kee-Tae1; Evans II,Neal J.1,5; Francesco,James Di6,7; Liu,Sheng-Yuan8; Yuan,Jinghua9; Tatematsu,Ken’ichi10; Zhang,Qizhou11; Ward-Thompson,Derek12; Fuller,Gary13; Goldsmith,Paul F.14; Koch,P. M.8; Sanhueza,Patricio10; Ristorcelli,I.15; Kang,Sung-ju1; Chen,Huei-Ru16; Hirano,N.8; Wu,Yuefang17; Sokolov,Vlas18; Lee,Chang Won1,19; White,Glenn J.20,21; Wang,Ke22; Eden,David23; Li,Di9,24; Thompson,Mark25; Pattle,Kate M16; Soam,Archana1; Nasedkin,Evert26; Kim,Jongsoo1; Kim,Gwanjeong10; Lai,Shih-Ping16; Park,Geumsook1; Qiu,Keping27; Zhang,Chuan-Peng9; Alina,Dana28; Eswaraiah,Chakali16; Falgarone,Edith29; Fich,Michel26; Greaves,Jane30; Gu,Q.-L.31; Kwon,Woojin1,19; Li,Hua-bai31; Malinen,Johanna32; Montier,Ludovic15; Parsons,Harriet2; Qin,Sheng-Li33; Rawlings,Mark G.2; Ren,Zhi-Yuan9; Tang,Mengyao33; Tang,Y.-W.8; Toth,L. V.34; Wang,Jiawei16; Wouterloot,Jan2; Yi,H.-W.35; Zhang,H.-W.17
Source PublicationThe Astrophysical Journal
AbstractAbstract 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 (FM), 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 FM is obtained using the Davis–Chandrasekhar–Fermi method. Based on 13CO (1–0) line observations, we suggest a formation scenario of FM due to large-scale (~10 pc) cloud–cloud collision. Using additional NH3 line data, we estimate that FM will be gravitationally unstable if it is only supported by thermal pressure and turbulence. The northern part of FM, however, can be stabilized by a modest additional support from the local magnetic field. The middle and southern parts of FM are likely unstable even if the magnetic field support is taken into account. We claim that the clumps in FM 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.
KeywordISM: clouds ISM: magnetic fields stars: formation
WOS IDIOP:0004-637X-859-2-aac025
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong-gu, Daejeon 34055, Republic of Korea;
2.East Asian Observatory, 660 N. A’ohoku Place, Hilo, HI 96720, USA
3.Astronomy Department, University of California, Berkeley, CA 94720, USA
4.Department of Physics, P.O. Box 64, FI-00014, University of Helsinki, Finland
5.Department of Astronomy, University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA
6.NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada
7.Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada
8.Institute of Astronomy and Astrophysics, Academia Sinica. 11F of Astronomy-Mathematics Building, AS/NTU No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan
9.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, People’s Republic of China
10.National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
11.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
12.Jeremiah Horrocks Institute for Mathematics, Physics & Astronomy, University of Central Lancashire, Preston PR1 2HE, UK
13.UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester M13 9PL, UK
14.Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
15.IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
16.Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan
17.Department of Astronomy, Peking University, 100871, Beijing, People’s Republic of China
18.Max Planck Institute for Extraterrestrial Physics, Gie?enbachstra?se 1, D-85748, Garching bei München, Germany
19.Korea University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea
20.Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes, MK7 6AA, UK
21.RAL Space, STFC Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire, OX11 0QX, UK
22.European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany
23.Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
24.Key Laboratory of Radio Astronomy, Chinese Academy of Science, Nanjing 210008, People’s Republic of China
25.Centre for Astrophysics Research, School of Physics Astronomy & Mathematics, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
26.Department of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 3G1, Canada
27.School of Astronomy and Space Science, Nanjing University, Nanjing 210023, People’s Republic of China
28.Department of Physics, School of Science and Technology, Nazarbayev University, Astana 010000, Kazakhstan
29.LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Ecole normale supérieure, F-75005 Paris, France
30.School of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UK
31.Department of Physics, The Chinese University of Hong Kong, Shatin, New Territory, Hong Kong, People’s Republic of China
32.Institute of Physics I, University of Cologne, Zülpicher Str. 77, D-50937, Cologne, Germany
33.Department of Astronomy, Yunnan University, and Key Laboratory of Astroparticle Physics of Yunnan Province, Kunming, 650091, People’s Republic of China
34.E?tv?s Loránd University, Department of Astronomy, Pázmány Péter sétány 1/A, H-1117, Budapest, Hungary
35.School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 17104, Republic of Korea
Recommended Citation
GB/T 7714
Liu,Tie,Li,Pak Shing,Juvela,Mika,et al. A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields[J]. The Astrophysical Journal,2018,859(2).
APA Liu,Tie.,Li,Pak Shing.,Juvela,Mika.,Kim,Kee-Tae.,Evans II,Neal J..,...&Zhang,H.-W..(2018).A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields.The Astrophysical Journal,859(2).
MLA Liu,Tie,et al."A Holistic Perspective on the Dynamics of G035.39-00.33: The Interplay between Gas and Magnetic Fields".The Astrophysical Journal 859.2(2018).
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