ID | 116823 |
タイトル別表記 | Dust polarization in OMC-1
|
著者 |
Pattle, Kate
National University of Ireland Galway|National Tsing Hua University
Lai, Shih-Ping
National Tsing Hua University|Academia Sinica Institute of Astronomy and Astrophysics
Wright, Melvyn
University of California
Coudé, Simon
Universities Space Research Association
Plambeck, Richard
University of California
Hoang, Thiem
Korea Astronomy and Space Science Institute|University of Science and Technology
Tang, Ya-Wen
Academia Sinica Institute of Astronomy and Astrophysics
Bastien, Pierre
Université de Montréal
Eswaraiah, Chakali
Chinese Academy of Sciences
Hwang, Jihye
Korea Astronomy and Space Science Institute|University of Science and Technology
Inutsuka, Shu-ichiro
Nagoya University
Kim, Kee-Tae
Korea Astronomy and Space Science Institute|University of Science and Technology
Kirchschlager, Florian
University College London
Kwon, Woojin
Seoul National University|Korea Astronomy and Space Science Institute
Lee, Chang Won
Korea Astronomy and Space Science Institute|University of Science and Technology
Liu, Sheng-Yuan
Academia Sinica Institute of Astronomy and Astrophysics
Lyo, Aran
Korea Astronomy and Space Science Institute
Ohashi, Nagayoshi
Academia Sinica Institute of Astronomy and Astrophysics
Rawlings, Mark G.
East Asian Observatory
Tahani, Mehrnoosh
National Research Council Canada
Tamura, Motohide
National Institutes of Natural Sciences|The University of Tokyo
Soam, Archana
Universities Space Research Association
Wang, Jia-Wei
Academia Sinica Institute of Astronomy and Astrophysics
Ward-Thompson, Derek
University of Central Lancashire
|
キーワード | techniques: polarimetric
stars: formation
ISM: dust, extinction
ISM: magnetic fields
submillimetre: ISM
|
資料タイプ |
学術雑誌論文
|
抄録 | We present ALMA Band 7 polarization observations of the OMC-1 region of the Orion molecular cloud. We find that the polarization pattern observed in the region is likely to have been significantly altered by the radiation field of the >104 L⊙ high-mass protostar Orion Source I. In the protostar’s optically thick disc, polarization is likely to arise from dust self-scattering. In material to the south of Source I – previously identified as a region of ‘anomalous’ polarization emission – we observe a polarization geometry concentric around Source I. We demonstrate that Source I’s extreme luminosity may be sufficient to make the radiative precession time-scale shorter than the Larmor time-scale for moderately large grains (>0.005−0.1μm), causing them to precess around the radiation anisotropy vector (k-RATs) rather than the magnetic field direction (B-RATs). This requires relatively unobscured emission from Source I, supporting the hypothesis that emission in this region arises from the cavity wall of the Source I outflow. This is one of the first times that evidence for k-RAT alignment has been found outside of a protostellar disc or AGB star envelope. Alternatively, the grains may remain aligned by B-RATs and trace gas infall on to the Main Ridge. Elsewhere, we largely find the magnetic field geometry to be radial around the BN/KL explosion centre, consistent with previous observations. However, in the Main Ridge, the magnetic field geometry appears to remain consistent with the larger-scale magnetic field, perhaps indicative of the ability of the dense Ridge to resist disruption by the BN/KL explosion.
|
掲載誌名 |
Monthly Notices of the Royal Astronomical Society
|
ISSN | 13652966
|
出版者 | Oxford University Press|The Royal Astronomical Society
|
巻 | 503
|
号 | 3
|
開始ページ | 3414
|
終了ページ | 3433
|
発行日 | 2021-03-04
|
権利情報 | This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
|
EDB ID | |
出版社版DOI | |
出版社版URL | |
フルテキストファイル | |
言語 |
eng
|
著者版フラグ |
出版社版
|
部局 |
教養教育院
|