论文标题
O-Type年轻恒星物体周围的磁盘
Disks around O-type young stellar objects
论文作者
论文摘要
积聚磁盘是恒星形成过程的关键要素之一。它们重新分配了角动量，并且在高质量恒星（M> 8msun）的情况下，磁盘将通过系统的电线杆通过辐射来减轻吸积材料的辐射压力，尤其是在赤道方向上，这将使积聚能够允许积聚进入中央门前（例如，Tan et al.G.，tan et al。实际上，近年来，所有高质量恒星理论似乎都融合到磁盘介导的吸积方案（例如，Krumholz等人2007； Kuiper等人，2011; Bonnell＆Bate 2006; Keto 2006; Keto 2007），但是高高的年轻Stellar对象（YSOS）是否可以确认该理论预测？还是换句话说，真正存在巨大恒星周围的真正积聚磁盘吗？
Accretion disks are one of the key ingredients of the star formation process. They redistribute angular momentum and, in the case of high-mass stars (M > 8Msun), disks would relieve the radiation pressure on the accreting material, in particular in the equatorial direction, by beaming the radiation through the poles of the system and this would allow the accretion to proceed onto the central protostar (e.g., Tan et al. 2014 for a review on massive star formation). In fact, in recent years, all high-mass star-forming theories appear to converge to a disk-mediated accretion scenario (e.g., Krumholz et al. 2007; Kuiper et al. 2011; Bonnell & Bate 2006; Keto 2007) but do the observations of high-mass young stellar objects (YSOs) confirm the theory predictions? Or in other words, do true accretion disks around massive stars really exist?
