论文标题
在太阳丝爆发期间确定He I10830Å中的动力学和磁场
Determining the dynamics and magnetic fields in He I 10830 Å during a solar filament eruption
论文作者
论文摘要
我们研究了等离子体的动力学和磁性特性，例如属于爆发的太阳丝的视线速度（LOS），光学深度，垂直和水平磁场。 2016年7月3日，在1.5米的Gregor望远镜处使用Gregor红外光谱仪（GRIS）观察到细丝爆发。在He I10830Å光谱范围内连续三次连续三连胜全孔散发丝光光谱扫描。使用机器学习K-均值算法对Stokes I配置文件进行了分类，然后使用Hazel Code倒入不同的初始条件。爆发的丝材料呈现以下物理条件：（1）峰值LOS速度约73 km/s的无处不在的向上运动； （2）磁场的主要大型水平成分，范围为173-254 g，而磁场的垂直成分平均要低得多，平均在39-58 g之间； （3）范围为0.7-1.1的光学深度。两次连续的栅格扫描（<2.5分钟）之间的场线的平均方位角取向保持恒定。分析的细丝喷发属于快速上升阶段，总速度约为124 km/s。磁场线的方向不会从一个栅格扫描到另一个光栅扫描，这表明尚未开始使用。灯丝爆发开始后约15分钟，不WIST的开始似乎开始了。
We investigate the dynamics and magnetic properties of the plasma, such as line-of-sight velocity (LOS), optical depth, vertical and horizontal magnetic fields, belonging to an erupted solar filament. The filament eruption was observed with the GREGOR Infrared Spectrograph (GRIS) at the 1.5-meter GREGOR telescope on 2016 July 3. Three consecutive full-Stokes slit-spectropolarimetric scans in the He I 10830 Å spectral range were acquired. The Stokes I profiles were classified using the machine learning k-means algorithm and then inverted with different initial conditions using the HAZEL code. The erupting-filament material presents the following physical conditions: (1) ubiquitous upward motions with peak LOS velocities of ~73 km/s; (2) predominant large horizontal components of the magnetic field, on average, in the range of 173-254 G, whereas the vertical components of the fields are much lower, on average between 39-58 G; (3) optical depths in the range of 0.7-1.1. The average azimuth orientation of the field lines between two consecutive raster scans (<2.5 minutes) remained constant. The analyzed filament eruption belonged to the fast rising phase, with total velocities of about 124 km/s. The orientation of the magnetic field lines does not change from one raster scan to the other, indicating that the untwisting phase has not started yet. The untwisting seems to start about 15 min after the beginning of the filament eruption.
