OBSERVATION OF THE EVOLUTION OF A CURRENT SHEET IN A SOLAR FLARE

被引：33

作者：

Zhu, Chunming ^{[1
]}

Liu, Rui ^{[2
,3
]}

Alexander, David ^{[4
]}

McAteer, R. T. James ^{[1
]}

机构：

[1] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA

[2] Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Peoples R China

[3] Collaborat Innovat Ctr Astronaut Sci & Technol, Changsha, Hunan, Peoples R China

[4] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2016年 / 821卷 / 02期

基金：

美国国家科学基金会;

关键词：

Sun: corona; Sun: flares; CORONAL MASS EJECTIONS; X-RAY TELESCOPE; MAGNETIC RECONNECTION; CHROMOSPHERIC EVAPORATION; HINODE; THICKNESS; OUTFLOWS; MISSION; INFLOW; REGION;

D O I：

10.3847/2041-8205/821/2/L29

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report multi-wavelength and multi-viewpoint observations of a solar eruptive event that involves loop-loop interactions. During a C2.0 flare, motions associated with inflowing and outflowing plasma provide evidence for ongoing magnetic reconnection. The flare loop top and a rising "concave-up" feature are connected by a current-sheet-like structure (CSLS). The physical properties (thickness, length, temperature, and density) of the CSLS are evaluated. In regions adjacent to the CSLS, the EUV emission (characteristic temperature at 1.6 MK) begins to increase more than 10 minutes prior to the onset of the flare, and steeply decreases during the decay phase. The reduction of the emission resembles that expected from coronal dimming. The dynamics of this event imply a magnetic reconnection rate in the range 0.01-0.05.

引用

页数：7

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