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arXiv 1306.6068astro-ph.SR
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He I D3对1984年5月22日M6太阳耀斑的观测

He I D3 Observation of the 1984 May 22 M6.3 Solar Flare

Chang Liu, Yan Xu, Na Deng, Jeongwoo Lee, Jifeng Zhang, Debi Prasad Choudhary, Haimin Wang

备注：
8 pages, 6 figures, accepted to the Astrophysical Journal
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摘要：

He I D3谱线对耀斑对低层大气的影响有独特的响应，可以作为能量输运过程的有力诊断工具。本文利用大熊座太阳天文台最近数字化的胶片图象，报道了1984年5月22日发生在具有圆形磁极性反转线（PIL）的活动区的M6.3耀斑的D3观测结果。耀斑的脉冲阶段始于一个在D3变暗的主要细长源，在其内部，明亮的发射核出现在硬X射线（HXR）的初始小峰值时。这些耀斑核心随后演变成一个尖锐的发射链，位于黑暗的晕内，同时在HXR的主峰，扭转了整体源对比度从-5%至5%。主峰期间D3的辐射能量估计约为10^30尔格，与20 keV以上的非热电子所携带的能量相当。之后，耀斑沿着圆形PIL逆时针方向前进，在D3中形成一个黑暗的圆形带，它显然反映了Ha和He I 10830 A中的明亮带。所有这些丝带持续超过一个小时的后期渐进阶段。我们认为，目前的事件类似于所谓的黑光耀斑，提出了基于连续图像，和D3变暗和变亮的功能，这里可能是由于，分别是热传导加热和高能电子的直接沉淀。

英文摘要：

He I D3 line has a unique response to the flare impact on the low solar atmosphere and can be a powerful diagnostic tool for energy transport processes. Using images obtained from the recently digitized films of Big Bear Solar Observatory, we report D3 observation of the M6.3 flare on 1984 May 22, which occurred in an active region with a circular magnetic polarity inversion line (PIL). The impulsive phase of the flare starts with a main elongated source that darkens in D3, inside of which bright emission kernels appear at the time of the initial small peak in hard X-rays (HXRs). These flare cores subsequently evolve into a sharp emission strand lying within the dark halo simultaneously with the main peak in HXRs, reversing the overall source contrast from -5% to 5%. The radiated energy in D3 during the main peak is estimated to be about 10^30 ergs, which is comparable to that carried by nonthermal electrons above 20 keV. Afterwards the flare proceeds along the circular PIL in the counterclockwise direction to form a dark circular ribbon in D3, which apparently mirrors the bright ribbons in Halpha and He I 10830 A. All these ribbons last for over one hour in the late gradual phase. We suggest that the present event resembles the so-called black-light flare that is proposed based on continuum images, and that D3 darkening and brightening features herein may be due to, respectively, the thermal conduction heating and the direct precipitation of high-energy electrons.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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