论文标题
喷出丝的磁性结构
Magnetic Structure of an Erupting Filament
论文作者
论文摘要
提出了喷发前太阳丝的完整3-D矢量磁场。在2017年5月29日和30日，在10830Å的邓恩太阳能望远镜处的设施红外光谱仪观察。在细丝中或附近发现了田间强度的双峰分布。平均场强度为24高斯，但在喷发之前，我们发现5月29日的观测值的第90个百分位数为435高斯。野外倾斜度距离太阳垂直距离约67度。场方位角与脊柱轴的角度约为47至65度。结果表明逆配置指示通量绳索拓扑。发现他的强度线与磁场方向共对准。灯丝的辛迪斯特构型如南半球所预期的。灯丝在2017年5月29日稳定，并在5月30日的两次观察中开始上升，然后爆发并导致较小的冠状质量弹出。在喷发过程中，磁拓扑没有明显变化。关于爆发细丝的磁性拓扑的此类信息可以改善太阳风暴的地球效果的预测。
The full 3-D vector magnetic field of a solar filament prior to eruption is presented. The filament was observed with the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope in the chromospheric He i line at 10830 Å on May 29 and 30, 2017. We inverted the spectropolarimetric observations with the HAnle and ZEeman Light (HAZEL) code to obtain the chromospheric magnetic field. A bimodal distribution of field strength was found in or near the filament. The average field strength was 24 Gauss, but prior to the eruption we find the 90th percentile of field strength was 435 Gauss for the observations on May 29. The field inclination was about 67 degree from the solar vertical. The field azimuth made an angle of about 47 to 65 degree to the spine axis. The results suggest an inverse configuration indicative of a flux rope topology. He i intensity threads were found to be co-aligned with the magnetic field direction. The filament had a sinistral configuration as expected for the southern hemisphere. The filament was stable on May 29, 2017 and started to rise during two observations on May 30, before erupting and causing a minor coronal mass ejection. There was no obvious change of the magnetic topology during the eruption process. Such information on the magnetic topology of erupting filaments could improve the prediction of the geoeffectiveness of solar storms.
