A topological approach to understand a multiple-loop solar flare
A topological approach to understand a multiple-loop solar flare
复制标题
理解多环太阳耀斑的拓扑方法
DOI：
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发表时间：
1995
期刊：
影响因子：
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通讯作者：
J. Hénoux
中科院分区：
文献类型：
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作者：
L. Bagalá;C. H. Mandrini;M. Rovira;P. Démoulin;J. Hénoux
我们分析了SMM卫星获得的1980年11月12日02：36 UT开始的AR 2779耀斑的紫外和X射线数据。从一个详细的修订Ov发射，我们发现，观察是兼容的能量被释放在一个区域以上的磁反转线的AR中间双极。然后，这种能量主要通过传导向位于AR主偶极中的两个远距离内核传输。本文首先确定了这些内核之一。加速粒子只在脉冲阶段对能量输运有贡献。我们通过离散的亚光球磁极对观测到的纵向磁场进行建模，并推导出磁场的整体拓扑。在以前的色球耀斑研究中，Ov核位于沿着计算的分界线与光球的交叉点。特别是在场线连接“不连续地”改变的情况下，这些核可以通过沿沿着分界线延伸的线成对地连接。我们的结果与磁重联在分界面上释放磁能的假设一致。
We analyze the UV and X-ray data obtained by the SMM satellite for the flare starting at 02:36 UT on November 12, 1980 in AR 2779. From a detailed revision of the Ov emission, we find that the observations are compatible with energy being released in a zone above the magnetic inversion line of the AR intermediate bipole. This energy is then transported mainly by conduction towards the two distant kernels located in the AR main bipole. One of these kernels is first identified in this paper. Accelerated particles contribute to the energy transport only during the impulsive phase.We model the observed longitudinal magnetic field by means of a discrete number of subphotospheric magnetic poles, and derive the magnetic field overall topology. As in previous studies of chromospheric flares, the Ov kernels are located along the intersection of the computed separatrices with the photosphere. Especially where the field-line linkage changes ‘discontinuously’, these kernels can be linked in pairs by lines that extend along separatrices. Our results agree with the hypothesis of magnetic energy released by magnetic reconnection occurring on separatrices.