Magnetic Stability of Massive Star-forming Clumps in RCW 106
Magnetic Stability of Massive Star-forming Clumps in RCW 106
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DOI：
10.3847/2041-8213/ab1346
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发表时间：
2019-04
期刊：
影响因子：
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通讯作者：
Shohei Tamaoki;K. Sugitani;Q. Nguyen-Luong;F. Nakamura;Takayoshi Kusune;T. Nagayama;Makoto Watanabe-Makoto-Watanab
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文献类型：
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作者：
Shohei Tamaoki;K. Sugitani;Q. Nguyen-Luong;F. Nakamura;Takayoshi Kusune;T. Nagayama;Makoto Watanabe-Makoto-Watanab
RCW 106分子云复合体是一个活跃的大质量恒星形成区域，那里正在发生迷你星暴。我们研究了它的磁结构的近红外偏振观测与成像偏振仪SIRPOL的IRSF 1.4米望远镜。全球磁场几乎平行于银道面和云伸长的方向。用Davis-Prasekhar-Fermi方法计算了71个团簇的磁场强度为100-1600 μG。我们还评估了这些团块的磁稳定性，发现大质量恒星形成团块往往是磁不稳定和引力不稳定的。因此，我们提出了一个新的标准来寻找大质量的恒星形成团块。这些细节表明，在不增加磁通量的情况下提高团块密度的过程对于大质量恒星的形成是必不可少的，并且是沿着磁力线吸积质量的必要性。
The RCW 106 molecular cloud complex is an active massive star-forming region where a ministarburst is taking place. We examined its magnetic structure by near-IR polarimetric observations with the imaging polarimeter SIRPOL on the IRSF 1.4 m telescope. The global magnetic field is nearly parallel to the direction of the Galactic plane and the cloud elongation. We derived the magnetic field strength of ∼100–1600 μG for 71 clumps with the Davis–Chandrasekhar–Fermi method. We also evaluated the magnetic stability of these clumps and found that massive star-forming clumps tend to be magnetically unstable and gravitationally unstable. Therefore, we propose a new criterion to search for massive star-forming clumps. These details suggest that the process enhancing the clump density without an increase of the magnetic flux is essential for the formation of massive stars and the necessity for accreting mass along the magnetic field lines.