Triggering Mechanism and Material Transfer of a Failed Solar Filament Eruption
文献类型：期刊论文
| 作者 | Yan,Xiaoli3,4,5; Xue,Zhike3,5; Cheng,Xin2; Zhang,Jun1 ; Wang,Jincheng3,5; Kong,Defang3,5; Yang,Liheng3,5; Chen,Guorong3,5; Feng,Xueshang4
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| 刊名 | The Astrophysical Journal
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| 出版日期 | 2020-01-29 |
| 卷号 | 889期号:2 |
| ISSN号 | 0004-637X |
| 关键词 | Sunspots Solar active region filaments Solar active region magnetic fields Solar activity Solar flares Solar magnetic fields Solar physics Solar atmosphere Solar filament eruptions Solar magnetic reconnection |
| DOI | 10.3847/1538-4357/ab61f3 |
| 英文摘要 | Abstract Solar filament eruptions are often associated with solar flares and coronal mass ejections, which have the greatest impact on space weather. However, the fine structures and the trigger mechanisms of solar filaments are still unclear. To address these issues, we studied a failed solar active-region filament eruption associated with a C-class flare by using high-resolution Hα images from the New Vacuum Solar Telescope, supplemented by EUV observations from the Solar Dynamics Observatory. Before the filament eruption, a small bipolar magnetic field emerged below the filament. Then magnetic reconnection between the filament and the emerging bipolar magnetic field triggered the filament eruption. During the filament eruption, the untwisting motion of the filament can be clearly traced by the eruptive threads. Moreover, the footpoints of the eruptive threads are determined by tracing the descending filament material. Note that the twisted structure of the filament and the right part of the eruptive filament threads cannot be seen before the filament eruption. These eruptive threads in the right part of the filament are found to be rooting in the weak negative polarities near the main negative sunspot. Moreover, a new filament formed in the filament channel due to material injection from the eruptive filament. The above observations and the potential field extrapolations are inclined to support the idea that the filament materials were transferred into the overlying magnetic loops and the nearby filament channel by magnetic reconnection. These observations improve our understanding of the complexity of filament eruptions. |
| 语种 | 英语 |
| 出版者 | The American Astronomical Society |
| WOS记录号 | IOP:0004-637X-889-2-AB61F3 |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/28751]  |
| 专题 | 中国科学院国家天文台 |
| 作者单位 | 1.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China 2.School of Astronomy and Space Science, Nanjing University, Nanjing 210093, People’s Republic of China 3.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, People’s Republic of China 4.Sate Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China 5.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People’s Republic of China; yanxl@ynao.ac.cn |
| 推荐引用方式 GB/T 7714 | Yan,Xiaoli,Xue,Zhike,Cheng,Xin,et al. Triggering Mechanism and Material Transfer of a Failed Solar Filament Eruption[J]. The Astrophysical Journal,2020,889(2). |
| APA | Yan,Xiaoli.,Xue,Zhike.,Cheng,Xin.,Zhang,Jun.,Wang,Jincheng.,...&Feng,Xueshang.(2020).Triggering Mechanism and Material Transfer of a Failed Solar Filament Eruption.The Astrophysical Journal,889(2). |
| MLA | Yan,Xiaoli,et al."Triggering Mechanism and Material Transfer of a Failed Solar Filament Eruption".The Astrophysical Journal 889.2(2020). |
入库方式： OAI收割
来源：国家天文台
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