Abstract Solar flare forecasting is limited by the current understanding of mechanisms that govern magnetic reconnection, the main physical phenomenon associated with these events. As a result, forecasting relies mainly on climatological correlations to historical events rather than the underlying physics principles. Solar physics models place the neutral point of the reconnection event in the solar corona. Correspondingly, studies of photospheric magnetic fields indicate changes during solar flares—particularly in relation to the field helicity—on the solar surface as a result of the associated magnetic reconnection. This study utilizes data from the Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager (HMI) and SpaceWeather HMI Active Region Patches (SHARPs) to analyze full vector-field component data of the photospheric magnetic field during solar flares within a large HMI dataset (May 2010 through September 2019). This analysis is then used to identify and compare trends in the different categories of flare strengths and determine indications of the physical phenomena taking place.

中文翻译：

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检测太阳耀斑中的重联特征

摘要 太阳耀斑预测受到当前对控制磁重联机制的理解的限制，磁重联是与这些事件相关的主要物理现象。因此，预测主要依赖于与历史事件的气候相关性，而不是基本的物理原理。太阳物理模型将重联事件的中性点置于日冕中。相应地，对光球磁场的研究表明，由于相关的磁重联，太阳耀斑期间太阳表面发生了变化——特别是与场螺旋度相关的变化。本研究利用来自太阳动力学天文台 (SDO) 日震和磁成像仪 (HMI) 和 SpaceWeather HMI 活动区域斑块 (SHARP) 的数据来分析大型 HMI 数据集内太阳耀斑期间光球磁场的完整矢量场分量数据2010 年 5 月至 2019 年 9 月）。然后使用该分析来识别和比较不同类别耀斑强度的趋势，并确定正在发生的物理现象的迹象。