论文标题
25 AU角度分辨率观察HH 211具有Alma：Sio，Co等的射流性质和冲击结构等
25 AU Angular Resolution Observations of HH 211 with ALMA : Jet Properties and Shock Structures in SiO, CO, and SO
论文作者
论文摘要
HH 211是一种高度准直的射流，在年轻的0级原始恒星的两侧都有一系列结和摆动结构。我们使用了两个时期的Atacama大毫米/亚毫米阵列（ALMA）数据，以$ \ sim $ 25 AU分辨率在CO（J = 3-2），SIO（j = 8-7）和SO（N_J = 8_9-7_8）线中研究其内部喷射。借助这些ALMA和以前的2008年亚易阵阵列（SMA）数据，发现中心来源的8节的适当动作是每年$ \ sim $ 0.068“每年$ \ sim $ 0.068”（$ \ sim $ \ sim $ \ sim $ 102 km/s），以前与$ \ sim $ \ sim $ \ sim forture fortive a forture fortive a fortroce a fortive a fortription。绕着射流源模型的旋转源。横向射击在该结中的位置 - 速度图中都被识别。
HH 211 is a highly collimated jet with a chain of knots and a wiggle structure on both sides of a young Class 0 protostar. We used two epochs of Atacama Large Millimeter/submillimeter Array (ALMA) data to study its inner jet in the CO(J=3-2), SiO(J=8-7), and SO(N_J=8_9-7_8) lines at $\sim$25 AU resolution. With these ALMA and previous 2008 Submillimeter Array (SMA) data, the proper motion of 8 knots within $\sim$250 AU of the central source is found to be $\sim$0.068" per year ($\sim$102 km/s), consistent with previous measurements in the outer jet. At $\sim$4 times higher resolution, the reflection-symmetric wiggle can be still fitted by a previously proposed orbiting jet source model. Previously detected continuous structures in the inner jet are now resolved, containing at least 5 sub-knots. These sub-knots are interpreted in terms of a variation in the ejection velocity of the jet with a period of $\sim$4.5 years, shorter than that of the outer knots. In addition, backward and forward shocks are resolved in a fully-formed knot, BK3, and signatures of internal working surface and sideways ejection are identified in Position-Velocity diagrams. In this knot, low-density SO and CO layers are surrounded by a high-density SiO layer.
