A RECONNECTING CURRENT SHEET IMAGED IN A SOLAR FLARE
A RECONNECTING CURRENT SHEET IMAGED IN A SOLAR FLARE
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DOI：
10.1088/2041-8205/723/1/l28
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发表时间：
2010-09
期刊：
影响因子：
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通讯作者：
Rui Liu;Jeongwoo Lee;Tongjiang Wang;G. Stenborg;Chang Liu;Haimin Wang
中科院分区：
文献类型：
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作者：
Rui Liu;Jeongwoo Lee;Tongjiang Wang;G. Stenborg;Chang Liu;Haimin Wang
磁场重联改变了磁场拓扑结构，并为天体物理、空间和实验室等离子体中的爆炸事件提供动力。对于太阳大气中的耀斑和日冕物质抛射（CME），标准模型预测存在重连电流片，这是过去50年来大量理论和数值模拟的主题，但缺乏直接，明确的观测验证。在这封信中，我们显示了一个明亮的片结构的全球长度（>0.25 R返）和宏观宽度（（5-10）×103公里）明显高于尖形耀斑环，在耀斑上升阶段的EUV成像。这片是由于跨赤道环系统的伸展而形成的，并伴随着各种重连特征。这一独特的事件提供了一个全面的看法，在太阳日冕的重联几何和动力学。
Magnetic reconnection changes the magnetic field topology and powers explosive events in astrophysical, space, and laboratory plasmas. For flares and coronal mass ejections (CMEs) in the solar atmosphere, the standard model predicts the presence of a reconnecting current sheet, which has been the subject of considerable theoretical and numerical modeling over the last 50 years, yet direct, unambiguous observational verification has been absent. In this Letter, we show a bright sheet structure of global length (>0.25 R☉) and macroscopic width ((5–10)×103 km) distinctly above the cusp-shaped flaring loop, imaged during the flare rising phase in EUV. The sheet formed due to the stretch of a transequatorial loop system and was accompanied by various reconnection signatures. This unique event provides a comprehensive view of the reconnection geometry and dynamics in the solar corona.