Quantitative Characterization of Magnetic Flux Rope Properties for Two Solar Eruption Events
Quantitative Characterization of Magnetic Flux Rope Properties for Two Solar Eruption Events
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DOI：
10.3847/1538-4357/ac78df
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发表时间：
2022-01
期刊：
影响因子：
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通讯作者：
W. He;Q. Hu;C. Jiang;J. Qiu;A. Prasad
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文献类型：
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作者：
W. He;Q. Hu;C. Jiang;J. Qiu;A. Prasad
为了弥补日冕物质抛射（cme）观测与日球层观测之间的差距，关键步骤之一是提高对其相应磁链（MFRs）等磁结构的理解。但是，由于缺乏对日冕磁场的直接测量，要确认日冕抛射爆发之前或之后是否存在相干的MFR，并定量地描述日冕抛射-MFR的特征，仍然是一个挑战。在这项研究中，我们研究了两个活跃区（AR）， AR 11719和AR 12158的MFR结构，并定量估计了它们的磁性能。我们使用预处理的光球矢量磁图进行非线性无力场外推。此外，利用遥感观测寻找太阳上MFRs的间接证据，并分析了与耀斑带相关的磁重联通量在喷发期间的时间演变。通过外推和观测相结合的分析，定量地确定了耀斑爆发前连贯的“预先存在的”MFR结构。在此基础上，估算了日冕物质抛射- mfr喷发前和喷发过程中两个太阳事件的磁通量特征，包括轴向磁通、磁场线扭曲和重联磁通，并与相应的原位模拟结果进行了比较。我们发现两个事件中伴随耀斑的磁重联为CME-MFRs喷发注入了大量的通量。
In order to bridge the gap between heliospheric and solar observations of coronal mass ejections (CMEs), one of the key steps is to improve the understanding of their corresponding magnetic structures like the magnetic flux ropes (MFRs). But it remains a challenge to confirm the existence of a coherent MFR before or upon the CME eruption on the Sun and to quantitatively characterize the CME-MFR due to the lack of direct magnetic field measurements in the corona. In this study, we investigate MFR structures originating from two active regions (ARs), AR 11719 and AR 12158, and estimate their magnetic properties quantitatively. We perform nonlinear force-free field extrapolations with preprocessed photospheric vector magnetograms. In addition, remote-sensing observations are employed to find indirect evidence of MFRs on the Sun and to analyze the time evolution of magnetic reconnection flux associated with the flare ribbons during the eruption. A coherent “preexisting” MFR structure prior to the flare eruption is identified quantitatively for one event from the combined analysis of the extrapolation and observation. Then the characteristics of MFRs for two events on the Sun before and during the eruption forming the CME-MFR, including the axial magnetic flux, field line twist, and reconnection flux, are estimated and compared with the corresponding in situ modeling results. We find that the magnetic reconnection associated with the accompanying flares for both events injects a significant amount of flux into the erupted CME-MFRs.