论文标题
从划分到扭曲的磁场在100 au等级中的过渡到0级Protostar B335
Transition from ordered pinched to warped magnetic field on a 100 au scale in the Class 0 protostar B335
论文作者
论文摘要
我们介绍了0.87毫米极化粉尘在0类Protostar B335中的观察结果，该灰尘发射以0.2“（20 au）分辨率获得的Atacama大毫米/亚毫米阵列（ALMA）获得的观察结果。我们将0.87 mm的数据与来自Alma存档的1.3 mm的数据进行了比较。在1.3毫米的系统上比0.87毫米的百分比高约1.7，这表明极化发射来自磁性排列的灰尘晶粒。赤道平面以及赤道平面的40-60度。由于磁场和旋转轴未对准的内部100 AU量表，B335的100个尺度可能会被扭曲，并且磁场可以被扭曲的积聚流拖动。
We present our observational results of the 0.87 mm polarized dust emission in the Class 0 protostar B335 obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at a 0.2" (20 au) resolution. We compared our data at 0.87 mm with those at 1.3 mm from the ALMA archive. The observed polarization orientations at the two wavelengths are consistent within the uncertainty, and the polarization percentages are systematically higher at 1.3 mm than 0.87 mm by a factor of ~1.7, suggesting that the polarized emission originates from magnetically aligned dust grains. We inferred the magnetic field orientations from the observed polarization orientations. We found that the magnetic field changes from ordered and highly pinched to more complicated and asymmetric structures within the inner 100 au scale of B335, and the magnetic field connects to the center along the equatorial plane as well as along the directions which are ~40-60 degrees from the equatorial plane. We performed non-ideal MHD simulations of collapsing dense cores. We found that similar magnetic field structures appear in our simulations of dense cores with the magnetic field and rotational axis slightly misaligned by 15 degrees but not in those with the aligned magnetic field and rotational axis. Our results suggest that the midplane of the inner envelope within the inner 100 au scale of B335 could be warped because of the misaligned magnetic field and rotational axis, and the magnetic field could be dragged by the warped accretion flows.
