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The Acceleration Process of a Solar Quiescent Filament in the Inner Corona
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; Song, H. Q., Email: hqsong@sdu.edu.cn
发表期刊ASTROPHYSICAL JOURNAL LETTERS
2018-04-20
卷号857期号:2
DOI10.3847/2041-8213/aabcc3
产权排序第5完成单位
收录类别SCI
关键词Instabilities Magnetic Reconnection Sun: Coronal Mass Ejections (Cmes) Sun: Flares
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
学科领域天文学
文章类型Article
ISSN2041-8205
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WOS记录号WOS:000430746100002
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]MAGNETIC-FIELD EVOLUTION ; MASS EJECTIONS ; ENERGY-RELEASE ; FLUX-ROPE ; ERUPTIVE FLARES ; 2-RIBBON FLARES ; RECONNECTION ; PROMINENCES ; INSTABILITY ; MODEL
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被引频次:1[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/12361
专题选址与日冕观测组
通讯作者Song, H. Q., Email: hqsong@sdu.edu.cn
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
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GB/T 7714
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).
APA Song, H. Q..,Chen, Y..,Qiu, J..,Chen, C. X..,Zhang, J..,...&Song, H. Q., Email: hqsong@sdu.edu.cn.(2018).The Acceleration Process of a Solar Quiescent Filament in the Inner Corona.ASTROPHYSICAL JOURNAL LETTERS,857(2).
MLA Song, H. Q.,et al."The Acceleration Process of a Solar Quiescent Filament in the Inner Corona".ASTROPHYSICAL JOURNAL LETTERS 857.2(2018).
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