A 16 au Binary in the Class 0 Protostar L1157 MMS
A 16 au Binary in the Class 0 Protostar L1157 MMS
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DOI：
10.3847/1538-4357/ac5594
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发表时间：
2022-02
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通讯作者：
J. Tobin;E. Cox;L. Looney
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作者：
J. Tobin;E. Cox;L. Looney
本文介绍了对0级原恒星L1157 MMS的甚大天线阵6.8mm和9mm波段的观测结果，分辨率为0.04 ″（14 Au）。我们检测到两个来源内L1157 MMS和解释这些来源作为一个二元原恒星与分离的16 Au。直接围绕在系统内部半径为50 Au的二元系统周围的物质的估计质量为0.11 M，根据观测到的尘埃排放量计算。我们解释所观察到的二元系统的背景下，其扁平的信封结构，低速率的信封旋转从5000至200 Au尺度，和一个有序的，极向磁场与流出对齐。因此，L1157 MMS是一个磁调节坍缩的原型系统，而L1157 MMS中存在一个紧凑的双星系统表明，在可能具有动态重要磁场的包层中仍然可以形成多颗星星。
We present Very Large Array observations toward the Class 0 protostar L1157 MMS at 6.8 and 9 mm with a resolution of ∼0.″04 (14 au). We detect two sources within L1157 MMS and interpret these sources as a binary protostar with a separation of ∼16 au. The material directly surrounding the binary system within the inner 50 au radius of the system has an estimated mass of 0.11 M ☉, calculated from the observed dust emission. We interpret the observed binary system in the context of previous observations of its flattened envelope structure, low rates of envelope rotation from 5000 to 200 au scales, and an ordered, poloidal magnetic field aligned with the outflow. Thus, L1157 MMS is a prototype system for magnetically regulated collapse, and the presence of a compact binary within L1157 MMS demonstrates that multiple star formation can still occur within envelopes that likely have dynamically important magnetic fields.