| Formation and Evolution of Transient Prominence Bubbles Driven by Erupting Minifilaments | |
Guo, Yilin1; Hou, Yijun2,3,4,5; Li, Ting2,3,5; Shen, Yuandeng6; Wang JC(王金成)4,7 ; Zhang, Jun8; Zheng, Jianchuan9; Wang, Dong9; Mei, Lin9
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| 发表期刊 | ASTROPHYSICAL JOURNAL
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| 2024-08-01 | |
| 卷号 | 970期号:2 |
| DOI | 10.3847/1538-4357/ad54b8 |
| 产权排序 | 第7完成单位 |
| 收录类别 | SCI |
| 摘要 | Prominence bubbles, the dark arch-shaped voids below quiescent prominences, are generally believed to be caused by the interaction between the prominences and the slowly emerging or quasi-stable underlying magnetic loops. However, this scenario could not explain some short-lived bubbles with extremely dynamic properties of evolution. Based on high-resolution H alpha observations, here we propose that bubbles should be classified into two categories according to their dynamic properties: quasi-steady Type-I bubbles and transient Type-II bubbles. Type-I bubbles could remain relatively stable and last for several hours, indicating the existence of a quasi-stable magnetic topology, while Type-II bubbles grow and collapse quickly within 1 hr without stability duration, which are usually associated with erupting minifilaments. Analysis of several typical Type-II bubbles from different views, especially including an on-disk event, reveals that Type-II bubbles quickly appear and expand at a velocity of similar to 5-25 km s-1 accompanied by an erupting minifilament below. The minifilament's rising velocity is slightly larger than that of the Type-II bubbles' boundary, which will lead to the collision with each other in a short time, subsequent collapse of Type-II bubbles, and formation of a large plume into the above prominence. We also speculate that only if the angle between the axis of the erupting minifilament and the line of sight is large enough, the interaction between the erupting minifilament and the overlying prominence could trigger a Type-II bubble with a typical arch-shaped but quickly expanding bright boundary. |
| 资助项目 | Strategic Priority Research Program of the Chinese Academy of Sciences[XDB0560000]; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB41000000]; BJAST Budding Talent Program[23CE-BGS-07]; National Natural Science Foundation of China[12273060]; National Natural Science Foundation of China[12222306]; National Natural Science Foundation of China[12073042]; National Natural Science Foundation of China[12173083]; National Natural Science Foundation of China[12003064]; National Natural Science Foundation of China[12073001]; Youth Innovation Promotion Association CAS[2023063]; National Key R&D Program of China[2022YFF0503800]; National Key R&D Program of China[2019YFA0405000]; Open Research Program of Yunnan Key Laboratory of Solar Physics and Space Science[YNSPCC202211]; Yunnan Science Foundation for Distinguished Young Scholars[202101AV070004]; Yunnan Key Laboratory of Solar Physics and Space Science[202205AG070009] |
| 项目资助者 | Strategic Priority Research Program of the Chinese Academy of Sciences[XDB0560000, XDB41000000] ; BJAST Budding Talent Program[23CE-BGS-07] ; National Natural Science Foundation of China[12273060, 12222306, 12073042, 12173083, 12003064, 12073001] ; Youth Innovation Promotion Association CAS[2023063] ; National Key R&D Program of China[2022YFF0503800, 2019YFA0405000] ; Open Research Program of Yunnan Key Laboratory of Solar Physics and Space Science[YNSPCC202211] ; Yunnan Science Foundation for Distinguished Young Scholars[202101AV070004] ; Yunnan Key Laboratory of Solar Physics and Space Science[202205AG070009] |
| 语种 | 英语 |
| 学科领域 | 天文学 ; 太阳与太阳系 |
| 文章类型 | Article |
| 出版者 | IOP Publishing Ltd |
| 出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
| ISSN | 0004-637X |
| URL | 查看原文 |
| WOS记录号 | WOS:001275398000001 |
| WOS研究方向 | Astronomy & Astrophysics |
| WOS类目 | Astronomy & Astrophysics |
| 关键词[WOS] | MAGNETIC-STRUCTURE ; FILAMENT-DRIVEN ; SOLAR |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 版本 | 出版稿 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/27495 |
| 专题 | 抚仙湖太阳观测和研究基地 |
| 作者单位 | 1.Beijing Planetarium, Beijing Academy of Science and Technology, Beijing 100044, People's Republic of China; 2.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China; [email protected]; 3.School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China; 4.Yunnan Key Laboratory of the Solar physics and Space Science, Kunming 650216, People's Republic of China; 5.State Key Laboratory of Solar Activity and Space Weather, Beijing 100190, People's Republic of China; 6.Shenzhen Key Laboratory of Numerical Prediction for Space Storm, Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen 518055, People's Republic of China; 7.Yunnan Observatories, Chinese Academy of Sciences, Kunming Yunnan 650216, People's Republic of China; 8.School of Physics and Optoelectronics Engineering, Anhui University, Hefei 230601, People's Republic of China; 9.Shenzhen Astronomical Observatory, Shenzhen 518040, People's Republic of China |
| 推荐引用方式 GB/T 7714 | Guo, Yilin,Hou, Yijun,Li, Ting,et al. Formation and Evolution of Transient Prominence Bubbles Driven by Erupting Minifilaments[J]. ASTROPHYSICAL JOURNAL,2024,970(2). |
| APA | Guo, Yilin.,Hou, Yijun.,Li, Ting.,Shen, Yuandeng.,王金成.,...&Mei, Lin.(2024).Formation and Evolution of Transient Prominence Bubbles Driven by Erupting Minifilaments.ASTROPHYSICAL JOURNAL,970(2). |
| MLA | Guo, Yilin,et al."Formation and Evolution of Transient Prominence Bubbles Driven by Erupting Minifilaments".ASTROPHYSICAL JOURNAL 970.2(2024). |
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