Dynamics of Late-stage Reconnection in the 2017 September 10 Solar Flare
Dynamics of Late-stage Reconnection in the 2017 September 10 Solar Flare
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DOI：
10.3847/1538-4357/aba94b
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发表时间：
2020-09-01
影响因子：
4.9
通讯作者：
Judge, Philip G.
中科院分区：
文献类型：
--
作者：
French, Ryan J.;Matthews, Sarah A.;Judge, Philip G.
在这篇多仪器论文中，我们寻找持续磁场重联的证据，远远超出了2017年9月10日X8.2级太阳耀斑的脉冲阶段。使用Hinode/EIS，CoMP，SDO/AIA，K-Cor，Hinode/XRT，RHESSI和IRIS，我们研究了耀斑动力学和拓扑结构的后期演化，与标准太阳耀斑模型预期的重连特征进行比较。检查以前未发表的EIS数据，我们提出了著名的等离子体片结构内的非热的速度和温度的演变，耀斑的持续时间的前四个小时。在更长的时间尺度上，我们使用差分发射测量和偏振数据来研究耀斑等离子体片和尖点结构的寿命，发现等离子体片在2017年9月11日的CoMP线性偏振观测中仍然可见，在其最后一次出现在EUV之后很久。我们推断，磁重联的某种形式仍在进行中，在这个时候-耀斑发作后27小时。
In this multi-instrument paper, we search for evidence of sustained magnetic reconnection far beyond the impulsive phase of the X8.2-class solar flare on 2017 September 10. Using Hinode/EIS, CoMP, SDO/AIA,K-Cor, Hinode/XRT, RHESSI, and IRIS, we study the late-stage evolution of the flare dynamics and topology, comparing signatures of reconnection with those expected from the standard solar flare model. Examining previously unpublished EIS data, we present the evolution of nonthermal velocity and temperature within the famous plasma sheet structure, for the first four hours of the flare's duration. On even longer timescales, we use differential emission measures and polarization data to study the longevity of the flare's plasma sheet and cusp structure, discovering that the plasma sheet is still visible in observations of CoMP linear polarization on 2017 September 11, long after its last appearance in EUV. We deduce that magnetic reconnection of some form is still ongoing at this time-27 hr after flare onset.