Two new schemes for identifying field lines involved in eruptions, the r-scheme and q-scheme, are proposed to analyze the eruptive and confined nature of solar flares, as extensions to the original r _m scheme proposed in Lin et al. Motivated by three solar flares originating from NOAA Active Region 12192 that are misclassified by r _m , we introduce refinements to the r-scheme employing the “magnetic twist flux” to approximate the force balance acting on a magnetic flux rope (MFR); in the q-scheme, the reconnected field is represented by those field lines that anchor in the flare ribbons. Based on data obtained by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, the coronal magnetic field for 51 flares larger than M5.0 class, from 29 distinct active regions, is constructed using a nonlinear force-free field extrapolation model. Statistical analysis based on linear discriminant function analysis is then performed, revealing that despite both schemes providing moderately successful classifications for the 51 flares, the coronal mass ejection-eruptivity classification for the three target events can only be improved with the q-scheme. We find that the highly twisted field lines and the flare-ribbon field lines have equal average force-free constant α, but all of the flare-ribbon-related field lines are shorter than 150 Mm in length. The findings lead us to conclude that it is challenging to distinguish the MFR from the ambient magnetic field using any quantity based on common magnetic nonpotentiality measures.

用于鉴定参与喷发场线的两个新方案中，- [R -scheme和q -scheme，提出了以分析太阳耀斑的喷发和密闭性，作为扩展到原始ř _米在Lin等人提出的方案。受来自 NOAA 活动区 12192 的三个太阳耀斑的驱动，这些耀斑被r _m错误分类，我们引入了对r方案的改进，采用“磁扭曲通量”来近似作用于磁通量绳 (MFR) 上的力平衡；在q -scheme，重新连接的场由锚定在耀斑带中的那些场线表示。根据太阳动力学天文台/日震和磁成像仪获得的数据，使用非线性无力场外推模型构建了来自 29 个不同活动区域的 51 个大于 M5.0 级耀斑的日冕磁场。然后进行基于线性判别函数分析的统计分析，表明尽管两种方案都为 51 次耀斑提供了适度成功的分类，但只有使用q方案才能改进三个目标事件的日冕物质抛射-爆发性分类。我们发现高度扭曲的场线和耀斑带场线具有相等的平均无力常数α，但所有与耀斑带相关的场线的长度都小于 150 毫米。这些发现使我们得出结论，使用基于常见磁非电势测量的任何量来区分 MFR 与环境磁场是具有挑战性的。