论文标题
使用高振动矢量磁图及其与耀斑丝带的关联，对太阳耀斑期间光球发生磁场变化的统计分析
A statistical Analysis of Magnetic Field Changes in the Photosphere During Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons
论文作者
论文摘要
我们分析了来自太阳能动力学观测站的37个耀斑的高效率磁力图（135〜S），并分析了闪光 - 丝梁观测，以了解光电矢量磁场变化的空间和时间特性及其与重新连接磁场的脚步点的关系。确认先前的研究，我们发现水平场成分的最大永久变化位于极性反转线附近，而垂直场的变化较不明显，并且分布在整个活动区域。我们发现，被丝带扫除的像素并不总是在田间表现出永久变化。但是，当它们这样做时，色带发射通常发生在田间变化开始前几分钟。该场的性质的变化与活动区域的大小没有关系，但与耀斑 - 丝带特性（如功能磁通通量和色带面积）密切相关。我们第一次发现，该场中永久变化的持续时间与耀斑的持续时间紧密相结合，平均持续29 \％的fo flare持续时间。我们的结果表明，光球磁场的变化是由两种情况的组合引起的：磁性重新连接和冠状内爆的耀斑收缩。
We analyze high-cadence vector magnetograms (135~s) and flare-ribbon observations of 37 flares from the Solar Dynamics Observatory to understand the spatial and temporal properties of changes in the photospheric vector magnetic field and their relationship to footpoints of reconnected fields. Confirming previous studies, we find that the largest permanent changes in the horizontal field component lie near the polarity inversion line, whereas changes in the vertical field are less pronounced and are distributed throughout the active region. We find that pixels swept up by ribbons do not always exhibit permanent changes in the field. However, when they do, ribbon emission typically occurs several minutes before the start of field changes. The changes in the properties of the field show no relation to the size of active regions, but are strongly related to the flare-ribbon properties such as ribbon magnetic flux and ribbon area. For the first time, we find that the duration of permanent changes in the field is strongly coupled with the duration of the flare, lasting on average 29\% of the duration of the GOES flare. Our results suggest that changes in photospheric magnetic fields are caused by a combination of two scenarios: contraction of flare loops driven by magnetic reconnection and coronal implosion.
