MAGNETIC FIELD STRUCTURE IN THE FLATTENED ENVELOPE AND JET IN THE YOUNG PROTOSTELLAR SYSTEM HH 211
MAGNETIC FIELD STRUCTURE IN THE FLATTENED ENVELOPE AND JET IN THE YOUNG PROTOSTELLAR SYSTEM HH 211
复制标题
年轻原恒星系统 HH 211 中扁平包层和喷流的磁场结构
DOI：
10.1088/2041-8205/797/1/l9
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
H. Hwang
中科院分区：
文献类型：
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作者：
Chin;R. Rao;T. Ching;S. Lai;N. Hirano;P. Ho;H. Hwang
HH 211是一个年轻的0类原恒星系统，有扁平的包层，可能有旋转盘和准直喷流。我们用亚毫米波阵在341.6GHz连续谱上和SiOJ = 8-7上以100.″6的分辨率对它进行了测绘。该连续谱追踪了扁平包层中的热尘埃发射和可能的圆盘。线性偏振检测在平坦的包络线中的连续。极化所暗示的场线有不同的方向，但它们与当前的引力坍缩模型并不矛盾，后者预测了取决于区域/距离的不同方向。此外，我们可能已经检测到的第一次偏振SiO线发射的射流由于Goldreich-Kylafis效应。需要在更高的灵敏度的观察，以确定在射流的字段形态。
HH 211 is a young Class 0 protostellar system with a flattened envelope, a possible rotating disk, and a collimated jet. We have mapped it with the Submillimeter Array in the 341.6 GHz continuum and SiO J = 8–7 at ∼0.″6 resolution. The continuum traces the thermal dust emission in the flattened envelope and the possible disk. Linear polarization is detected in the continuum in the flattened envelope. The field lines implied from the polarization have different orientations, but they are not incompatible with current gravitational collapse models, which predict a different orientation depending on the region/distance. Also, we might have detected for the first time polarized SiO line emission in the jet due to the Goldreich–Kylafis effect. Observations at higher sensitivity are needed to determine the field morphology in the jet.