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题名:
The Acceleration Process of a Solar Quiescent Filament in the Inner Corona
作者: Song, H. Q.1; Chen, Y.1; Qiu, J.2; Chen, C. X.1; Zhang, J.3; Cheng, X.4; Shen YD(申远灯)5; Zheng, R. S.1
刊名: ASTROPHYSICAL JOURNAL LETTERS
出版日期: 2018-04-20
卷号: 857, 期号:2
DOI: 10.3847/2041-8213/aabcc3
学科分类: 天文学
产权排序: 第5完成单位
收录类别: SCI
通讯作者: Song, H. Q., Email: hqsong@sdu.edu.cn
关键词: instabilities ; magnetic reconnection ; Sun: coronal mass ejections (CMEs) ; Sun: flares
英文摘要: Coronal mass ejections (CMEs) are frequently associated with filament eruptions. Theoretical studies propose that both magnetic reconnection and ideal magnetohydrodynamic instability of magnetic flux ropes can convert coronal magnetic energy into the filament/CME kinetic energy. Numerical simulations and analytical considerations demonstrate that both mechanisms can have significant contributions to the filament/CME acceleration. Many observational studies support that reconnection plays an important role during the acceleration, while it remains open how to resolve observationally the contribution of the ideal instability to the acceleration. On the other hand, it is difficult to separate and compare their contributions through observations as both mechanisms often work in a close time sequence. In this Letter, the above issues are addressed by analyzing the eruption process of a quiescent filament. The filament started to rise from similar to 00:00 UT on 2011 December 25, 20 minutes earlier than the starting time of the flare impulsive phase (similar to 00:20 UT), and reached the maximum velocity at the flare peak time (similar to 00:50 UT). We divide the acceleration process into two stages, corresponding to the pre-flare and flare impulsive phases, respectively. The analysis indicates that an ideal flux-rope instability is dominant in the first stage, while reconnection below the flux rope becomes important during the second stage, and both mechanisms may have comparable contributions to the net acceleration of the filament.
项目资助者: Shandong Provincial Natural Science Foundation(JQ201710) ; National Natural Science Foundation of China (NSFC)(U1731102, U1731101) ; Chinese Academy of Sciences (CAS) ; NSFC(41331068, 11790303, 11790300) ; CAS(XDA-17040505, XDA-15010900)
语种: 英语
原文出处: 查看原文
ISSN号: 2041-8205
文章类型: Article
WOS标题词: Science & Technology ; Physical Sciences
研究领域[WOS]: Astronomy & Astrophysics
类目[WOS]: Astronomy & Astrophysics
关键词[WOS]: MAGNETIC-FIELD EVOLUTION ; MASS EJECTIONS ; ENERGY-RELEASE ; FLUX-ROPE ; ERUPTIVE FLARES ; 2-RIBBON FLARES ; RECONNECTION ; PROMINENCES ; INSTABILITY ; MODEL
WOS记录号: WOS:000430746100002
Citation statistics:
内容类型: 期刊论文
URI标识: http://ir.ynao.ac.cn/handle/114a53/12361
Appears in Collections:选址与日冕观测组_期刊论文

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作者单位: 1.Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209, People's Republic of China
2.Department of Physics, Montana State University, Bozeman, MT 59717, USA
3.Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030, USA
4.School of Astronomy and Space Science, Nanjing University, Nanjing, Jiangsu 210093, People's Republic of China
5.Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650216, People's Republic of China

Recommended Citation:
Song, H. Q.,Chen, Y.,Qiu, J.,et al. The Acceleration Process of a Solar Quiescent Filament in the Inner Corona[J]. ASTROPHYSICAL JOURNAL LETTERS,2018,857(2).
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