A formation mechanism for the large plumes in the prominence | |
Wang JC(王金成)3,4,5; Yan XL(闫晓理)4,5; Xue ZK(薛志科)4,5; Yang LH(杨丽恒)4,5; Li, Qiaoling6; Chen, Hechao1; Xia, Chun2; Liu Z(刘忠)4,5 | |
刊名 | ASTRONOMY & ASTROPHYSICS |
2022-03-09 | |
卷号 | 659 |
关键词 | Sun: filaments, prominences Sun: corona |
ISSN号 | 0004-6361 |
DOI | 10.1051/0004-6361/202142584 |
产权排序 | 第1完成单位 |
文献子类 | Article |
英文摘要 | Aims. To understand the formation mechanism of large plumes in solar prominences, we investigate the formation process of two such phenomena. Methods. We studied the dynamic and thermal properties of two large plumes using observations from New Vacuum Solar Telescope, the Solar Dynamic Observatory, and the Solar Terrestrial Relations Observatory-Ahead. We employed the differential emission measures method to diagnose the thermodynamical nature of the bubble and plumes. We calculated the Doppler signals based on observations of Ha blue and red wings. Results. We find that two large plumes observed with high-resolution data are quite different from previously studied small-scale plumes. They are born at the top of a prominence bubble with a large projected area of 10-20 Mm(2). Before the occurrence of each large plume, the bubble expands and takes on a quasi-semicircular appearance. Meanwhile, the emission intensity of extreme-ultraviolet bands increases in the bubble. A small-scale filament is found to erupt in the bubble during the second large plume. At the point at which the height of the bubble is comparable with half the width of the bubble, the bubble becomes unstable and generates the plumes. During the formation of plumes, two side edges of the top of the bubble, which are dominated by opposite Doppler signals, approach each other. The large plume then emerges and keeps rising up with a constant speed of about 13-15 km s(-1). These two large plumes have temperatures of similar to 1.3 x 10(6) K and densities of similar to 2.0 x 10(9) cm(-3), two orders hotter and one order less dense than the typical prominence. We also find that the bubble is a hot, low-density volume instead of a void region beneath the cold and dense prominence. Conclusions. These two large plumes are the result of the breakup of the prominence bubble triggered by an enhancement of thermal pressure; they separate from the bubble, most likely by magnetic reconnection. |
学科主题 | 天文学 ; 太阳与太阳系 ; 太阳物理学 |
URL标识 | 查看原文 |
出版地 | 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE |
资助项目 | National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12003064] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11873087] ; National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[11803085] ; Yunnan Science Foundation of China[2019FD085] ; National Key R&D Program of China[2019YFA0405000] ; CAS Light of West China Program[Y9XB018001] ; Open Research Program of the Key Laboratory of Solar Activity of Chinese Academy of Sciences[KLSA202014] ; Yunnan Talent Science Foundation of China[2018FA001] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Research and Development Project of Yunnan Province[202003AD150019] |
WOS关键词 | MAGNETIC-STRUCTURE ; SOLAR ; DENSITY ; FLOWS ; RECONNECTION ; INSTABILITY ; TOPOLOGY ; BUBBLES ; MOTION ; FIELD |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | EDP SCIENCES S A |
WOS记录号 | WOS:000766307300004 |
资助机构 | National Science Foundation of China (NSFC)National Natural Science Foundation of China (NSFC)[12003064, 11873087, 11803085] ; Yunnan Science Foundation of China[2019FD085] ; National Key R&D Program of China[2019YFA0405000] ; CAS Light of West China Program[Y9XB018001] ; Open Research Program of the Key Laboratory of Solar Activity of Chinese Academy of Sciences[KLSA202014] ; Yunnan Talent Science Foundation of China[2018FA001] ; Yunnan Science Foundation for Distinguished Young Scholars[202001AV070004] ; Key Research and Development Project of Yunnan Province[202003AD150019] |
内容类型 | 期刊论文 |
版本 | 出版稿 |
源URL | [http://ir.ynao.ac.cn/handle/114a53/24981] |
专题 | 云南天文台_抚仙湖太阳观测站 |
通讯作者 | Wang JC(王金成) |
作者单位 | 1.School of Earth and Space Sciences, Peking University, Beijing 100871, PR China; 2.School of Physics and Astronomy, Yunnan University, Kunming 650050, PR China 3.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Beijing 100012, PR China; 4.Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650216, PR China; 5.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China; 6.Department of Physics, Yunnan University, Kunming 650091, PR China; |
推荐引用方式 GB/T 7714 | Wang JC,Yan XL,Xue ZK,et al. A formation mechanism for the large plumes in the prominence[J]. ASTRONOMY & ASTROPHYSICS,2022,659. |
APA | Wang JC.,Yan XL.,Xue ZK.,Yang LH.,Li, Qiaoling.,...&Liu Z.(2022).A formation mechanism for the large plumes in the prominence.ASTRONOMY & ASTROPHYSICS,659. |
MLA | Wang JC,et al."A formation mechanism for the large plumes in the prominence".ASTRONOMY & ASTROPHYSICS 659(2022). |
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