A CHANGE OF ROTATION PROFILE IN THE ENVELOPE IN THE HH 111 PROTOSTELLAR SYSTEM: A TRANSITION TO A DISK?
A CHANGE OF ROTATION PROFILE IN THE ENVELOPE IN THE HH 111 PROTOSTELLAR SYSTEM: A TRANSITION TO A DISK?
复制标题
HH 111 原恒星系统外壳旋转轮廓的变化：向圆盘的过渡？
DOI：
10.1088/0004-637x/725/1/712
复制
发表时间：
2010
期刊：
影响因子：
--
通讯作者：
Chin
中科院分区：
文献类型：
--
作者：
Chin
HH 111 原恒星系统由两个 I 类源（VLA 1 和 2）组成，推定盘深深嵌入扁平包络中，距离为 400 pc。对该系统在 C18O (J = 2–1)、SO (NJ = 56–45) 和 1.33 mm 连续体中以 ~1" (400 AU) 分辨率进行了后续研究，它可能首次展示如何在下落的包络线内形成旋转支撑的圆盘。 1.33 毫米的连续辐射是由两个源头产生的，很可能追踪它们周围布满尘埃的假定圆盘。特别是，VLA 1 源周围的发射在赤道面内被拉长，半径为~300 AU。包络在 C18O 中清晰可见，从 VLA 1 源延伸至~7000 AU，最里面的部分与布满灰尘的圆盘重叠。它具有微分旋转，外部（∼2000–7000 AU）可以通过具有恒定比角动量的旋转更好地描述，而内部（∼60–2000 AU）则可以通过开普勒旋转更好地描述。包络线似乎也有一些小于旋转运动的坠落运动。因此，外壳外部的材料似乎以其角动量缓慢向内螺旋旋转，而内部的旋转确实可以变成开普勒式。在半径约为 400 AU 的 VLA 1 源周围可以看到紧凑的 SO 发射，它可能追踪诸如盘周围的（内部）吸积激波之类的激波。
The HH 111 protostellar system consists of two Class I sources (VLA 1 and 2) with putative disks deeply embedded in a flattened envelope at a distance of 400 pc. A follow-up study of this system in C18O (J = 2–1), SO (NJ = 56–45), and 1.33 mm continuum at ∼1″ (400 AU) resolution is performed, and it may show for the first time how a rotationally supported disk can be formed inside an infalling envelope. The 1.33 mm continuum emission is seen arising from both sources, likely tracing the dusty putative disks around them. In particular, the emission around the VLA 1 source is elongated in the equatorial plane with a radius of ∼300 AU. The envelope is well seen in C18O, extending to ∼7000 AU out from the VLA 1 source, with the innermost part overlapping with the dusty disk. It has a differential rotation, with the outer part (∼2000–7000 AU) better described by a rotation that has constant specific angular momentum and the inner part (∼60–2000 AU) by a Keplerian rotation. The envelope seems to also have some infall motion that is smaller than the rotation motion. Thus, the material in the outer part of the envelope seems to be slowly spiraling inward with its angular momentum and the rotation can indeed become Keplerian in the inner part. A compact SO emission is seen around the VLA 1 source with a radius of ∼400 AU and it may trace a shock such as an (inner) accretion shock around the disk.