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题名: On a Solar Blowout Jet: Driving Mechanism and the Formation of Cool and Hot Components
作者: Shen, Yuandeng; Liu, Ying D.; Su, Jiangtao; Qu, Zhining; Tian, Zhanjun
作者部门: 空间科学部
通讯作者: Shen, YD (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China. ; Shen, YD (reprint author), Chinese Acad Sci, State Key Lab Space Weather, Beijing 100190, Peoples R China. ; Shen, YD (reprint author), Chinese Acad Sci, Key Lab Solar Act, Natl Astron Observ, Beijing 100012, Peoples R China. ; Shen, YD (reprint author), Chinese Acad Sci, Ctr Astron Mega Sci, Beijing 100012, Peoples R China.
关键词: Sun: activity ; Sun: filaments ; prominences ; Sun: flares ; Sun: magnetic fields Supporting material: animation
刊名: ASTROPHYSICAL JOURNAL
ISSN号: 0004-637X
出版日期: 2017
卷号: 851, 期号:1, 页码:67
收录类别: SCI
项目资助者: Natural Science Foundation of China [11403097, 11633008, 11773068] ; Yunnan Science Foundation [2015FB191, 2017FB006] ; Specialized Research Fund for State Key Laboratories ; Open Research Program of the Key Laboratory of Solar Activity of Chinese Academy of Sciences [KLSA201601] ; Youth Innovation Promotion Association of Chinese Academy of Sciences [2014047]
英文摘要: We present observations of a blowout jet that experienced two distinct ejection stages. The first stage started from the emergence of a small positive magnetic polarity, which was cancelled by the nearby negative magnetic field and caused the rising of a mini-filament and its confining loops. This further resulted in a small jet due to the magnetic reconnection between the rising confining loops and the overlying open field. The second ejection stage was mainly due to successive removal of the confining field by reconnection: the filament erupted, and the erupting cool filament material directly combined with the hot jet that originated form the reconnection region and therefore formed the cool and hot components of the blowout jet. During the two ejection stages, cool Ha jets are also observed cospatial with their coronal counterparts, but their appearance times are earlier by a few minutes than those of the hot coronal jets. The hot coronal jets are therefor possibly caused by the heating of the cool Ha jets or the rising of the reconnection height from the chromosphere to the corona. The scenario that magnetic reconnection occurred between the confining loops and the overlying open loops is supported by many observational facts, including the bright patches on both sides of the mini-filament, hot plasma blobs along the jet body, and periodic metric radio type III bursts at the very beginnings of the two stages. The evolution and characteristics of these features show the detailed nonlinear process in magnetic reconnection.
语种: 英语
内容类型: 期刊论文
URI标识: http://ir.nssc.ac.cn/handle/122/6117
Appears in Collections:空间科学部_期刊论文

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