用速度矢量揭示巨蛇座G3-G6分子云的引力坍缩
Revealing Gravitational Collapse in Serpens G3-G6 Molecular Cloud using Velocity Gradients
摘要：
湍流、磁场、自引力在恒星形成中的相对作用是一个激烈争论的主题。本文介绍了IRAM 30 m望远镜对巨蛇座G3-G6分子云中$^{13}$ CO（1-0）发射的观测，并对观测数据应用了一套统计方法。其中包括柱密度的概率密度函数（PDF）和速度梯度技术（VGT）。我们结合我们的数据与普朗克353 GHz极化尘埃发射观测，赫谢尔H $_2$柱密度。我们认为巨蛇座G3-G6南星团正在经历一次引力坍缩。我们的分析表明引力坍缩发生在体积密度$n\ge10^3$ $\rm cm^{-3}$。我们使用传统的Davis-Davrasekhar-Fermi方法估计了大约120个$μG$的天空平面磁场强度，使用Lazarian等人提出的新技术估计了100个$μG$的天空平面磁场强度。（2020年）。我们发现巨蛇座G3-G6南星系团的总磁场能量明显超过动能和引力能。我们的结论是，引力坍缩可以成功地触发在超音速和亚阿尔夫文云。
英文摘要：
The relative role of turbulence, magnetic fields, self-gravity in star formation is a subject of intensive debate. We present IRAM 30m telescope observations of the $^{13}$CO (1-0) emission in the Serpens G3-G6 molecular cloud and apply to the data a set of statistical methods. Those include the probability density functions (PDFs) of column density and the Velocity Gradients Technique (VGT). We combine our data with the Planck 353 GHz polarized dust emission observations, Hershel H$_2$ column density. We suggest that the Serpens G3-G6 south clump is undergoing a gravitational collapse. Our analysis reveals that the gravitational collapse happens at volume density $n\ge10^3$ $\rm cm^{-3}$. We estimate the plane-of-the-sky magnetic field strength of approximately 120 $μG$ using the traditional Davis-Chandrasekhar-Fermi method and 100 $μG$ using a new technique proposed in Lazarian et al.(2020). We find the Serpens G3-G6 south clump's total magnetic field energy significantly surpasses kinetic energy and gravitational energy. We conclude that the gravitational collapse could be successfully triggered in a supersonic and sub-Alfvénic cloud.
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