期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 503, 期 3, 页码 3414-3433出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab608
关键词
techniques: polarimetric; stars: formation; ISM: dust, extinction; ISM: magnetic fields; submillimetre: ISM
资金
- Ministry of Science and Technology (MOST), Taiwan [106-2119-M-007-021-MY3, 109-2112M-007-010-MY3, 108-2112-M-001-004-MY2]
- SOFIA Science Center
- National Aeronautics and Space Administration [NNA17BF53C]
- National Research Foundation of Korea (NRF) - Korean government (MSIT) [2019R1A2C1087045]
- Basic Science Research Program through the NRF - Ministry of Education, Science and Technology [NRF-2019R1A2C1010851]
- East Asian Observatory
- NASA Astrophysics Data System
ALMA Band 7 polarization observations of the OMC-1 region of the Orion molecular clouds showed that the polarization pattern was influenced by the radiation field of the high-mass protostar Orion Source I. The optically thick disc of the protostar likely caused polarization from dust self-scattering, revealing a concentric geometry around Source I. The extreme luminosity of Source I may cause grains to precess around the radiation anisotropy vector, supporting the emission from the Source I outflow cavity wall.
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 >10(4) L-circle dot 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 (> 0.005-0.1 mu m), 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.
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