论文标题
2017年9月10日太阳能耀斑的晚期重新连接的动力
Dynamics of Late-Stage Reconnection in the 2017 September 10 Solar Flare
论文作者
论文摘要
在这篇多功能列表的论文中，我们在2017年9月10日的X8.2级太阳能耀斑的冲动阶段远远超出了持续的磁重新连接的证据。使用HINODE/EIS，COMP，SDO/AIA，K-COR，HINODE/HINODE/HINODE/HINODE/HINODE/RHEST，RHESSI，RHESSI，RHESSI和IRIS与这些预期的杂物相比，我们研究了这些预期的杂物。 模型。在检查以前未发表的EIS数据时，我们介绍了著名的浆片结构内的非热速度和温度的演变，在耀斑持续时间的前四个小时。在更长的时间尺度上，我们使用差分排放度量和极化数据来研究耀斑的浆片和尖尖结构的寿命，发现在2017年9月11日的Comp Lineal极化观察结果中，在其最后一次出现在EUV中的COMP线性极化观察中仍然可以看到等离子体表。我们推断出某种形式的磁重新连接目前仍在进行中 - 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 Examining previously unpublished EIS data, we present the evolution of non-thermal velocity and temperature within the famous plasma sheet structure, for the first four hours of the flare's duration. On even longer time scales, 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 CoMP linear polarization observations 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 hours after flare onset.
