太阳爆发活动区的磁复杂性与爆发参数
Magnetic Complexity in Eruptive Solar Active Regions and Associated Eruption Parameters
摘要：
使用一个有效的磁复杂性指数在活动区的太阳光球，我们量化的耀斑前强度的光球磁极性反转线在23个喷发活动区的耀斑/CME/ICME事件跟踪所有的方式从太阳到地球。我们发现，更强烈的极性反转线的活动区主机统计更强的耀斑和更快，更冲动地加速，CME。没有显着的相关性之间的强度的反演线和耀斑软X射线上升时间，ICME过境时间，和峰值$Dst指数的诱发磁暴。证实这些和以前的结果，我们推测源活动区，耀斑和日冕物质抛射之间的连接可能的解释。需要进一步的工作来验证这一概念并揭示其物理细节。
英文摘要：
Using an efficient magnetic complexity index in the active-region solar photosphere, we quantify the preflare strength of the photospheric magnetic polarity inversion lines in 23 eruptive active regions with flare/CME/ICME events tracked all the way from the Sun to the Earth. We find that active regions with more intense polarity inversion lines host statistically stronger flares and faster, more impulsively accelerated, CMEs. No significant correlation is found between the strength of the inversion lines and the flare soft X-ray rise times, the ICME transit times, and the peak $Dst indices of the induced geomagnetic storms. Corroborating these and previous results, we speculate on a possible interpretation for the connection between source active regions, flares, and CMEs. Further work is needed to validate this concept and uncover its physical details.
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