IMAGING A MAGNETIC-BREAKOUT SOLAR ERUPTION
IMAGING A MAGNETIC-BREAKOUT SOLAR ERUPTION
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DOI：
10.3847/2041-8205/820/2/l37
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发表时间：
2016-03
期刊：
影响因子：
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通讯作者：
Yao Chen;G. Du;Di Zhao;Zhao Wu;Wei Liu;B. Wang;G. Ruan;S. Feng;Hongqiang Song
中科院分区：
文献类型：
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作者：
Yao Chen;G. Du;Di Zhao;Zhao Wu;Wei Liu;B. Wang;G. Ruan;S. Feng;Hongqiang Song
引发日冕物质抛射（CME）的基本机制仍然存在争议。其中一个主要的理论是磁爆发，其中在日冕中发生的磁重联从上覆的磁场中消除了对通电的低日冕结构的限制，从而使其爆发。在这里，我们报告的关键观测证据，这种难以捉摸的突破重联在多极磁配置，导致CME和X级，长时间的耀斑。它的发生是由周围的X型零点和重联流入签名加热尖形环对的存在下支持。突破图片的其他奇特特征包括连续环增亮，能量高达100keV的日冕硬X射线，以及后来恢复的多极结构上方的扩展高日冕X射线。这些观测，从一个新的角度与清晰度从来没有实现过，目前的关键线索，了解太阳爆发的启动机制。
The fundamental mechanism initiating coronal mass ejections (CMEs) remains controversial. One of the leading theories is magnetic breakout, in which magnetic reconnection occurring high in the corona removes the confinement on an energized low-corona structure from the overlying magnetic field, thus allowing it to erupt. Here, we report critical observational evidence of this elusive breakout reconnection in a multi-polar magnetic configuration that leads to a CME and an X-class, long-duration flare. Its occurrence is supported by the presence of pairs of heated cusp-shaped loops around an X-type null point and signatures of reconnection inflows. Other peculiar features new to the breakout picture include sequential loop brightening, coronal hard X-rays at energies up to ∼100 keV, and extended high-corona X-rays above the later restored multi-polar structure. These observations, from a novel perspective with clarity never achieved before, present crucial clues to understanding the initiation mechanism of solar eruptions.