论文标题
通过检测射流底座的径向流动验证的原始喷气机磁中心的起源
Magneto-Centrifugal Origin for Protostellar Jets Validated through Detection of Radial Flow at the Jet Base
论文作者
论文摘要
喷气机可以在恒星形成中促进质量积聚。据信，它们是通过磁性中心力量从质子周围的积聚磁盘发射的，这是由其中一些旋转和磁场的检测支持的。在这里，我们报告了基部的教科书案例Protostellar Jet HH 212的径向流动，以进一步支持这种喷出的场景。这种径向流验证了射流形成和准直的磁心中心理论的核心预测，即，射流是广角风的最密集的部分，在远距离远距离向外流动的广角风中，距离（小，sub-au）发射区域。径向流动的广角分量的其他证据来自其在HH 212射流周围检测到的壳的结构和运动学的能力。该组件可以将材料从内部磁盘传输到外盘，可以解释在太阳系中在大距离内检测到的软骨和富含的夹杂物。
Jets can facilitate the mass accretion onto the protostars in star formation. They are believed to be launched from accretion disks around the protostars by magneto-centrifugal force, as supported by the detections of rotation and magnetic field in some of them. Here we report a radial flow of the textbook-case protostellar jet HH 212 at the base to further support this jet-launching scenario. This radial flow validates a central prediction of the magneto-centrifugal theory of jet formation and collimation, namely, the jet is the densest part of a wide-angle wind that flows radially outward at distances far from the (small, sub-au) launching region. Additional evidence for the radially flowing wide-angle component comes from its ability to reproduce the structure and kinematics of the shells detected around the HH 212 jet. This component, which can transport material from inner to outer disk, could account for the chondrules and Ca-Al-rich inclusions detected in the Solar System at large distances.
