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Formation and Dynamics in an Observed Preeruptive Filament

文献类型：期刊论文

作者Huang, Jing1,2,5; Zhang, Yin1,5; Tan, Baolin1,2,5; Bai, Xianyong1,2,5; Li, Leping1,5; Hou, Zhenyong3; Yang, Xiao1,5; Ji KF(季凯帆)4; Song, Yongliang1,5; Hu, Ziyao1,2,5
刊名ASTROPHYSICAL JOURNAL LETTERS
出版日期2023-11-01
卷号958期号:1
ISSN号2041-8205
DOI10.3847/2041-8213/ad083e
产权排序第5完成单位
文献子类Article
英文摘要The formation of filaments/prominences is still a debated topic. Many different processes have been proposed: levitation, injection of cool plasma, merging filaments, and cooling plasma in hot loops. We take the opportunity to make a multiwavelength analysis of the formation of an active-region filament, combining several UV and EUV observations including the new Ne vii 465 angstrom filtergrams provided by the Solar Upper Transition Region Imager on board the Space Advanced Technology satellite. The filament is mainly observed at the limb for 3 hr. It is progressively formed through a series of stages, including emergence and cooling of hot loops, reconnection between small filaments, material transfer in a large filament channel, and reconnection between filaments and emerged hot loops. From the observations at 465 angstrom, we find that the new-formed filaments show bright structures as in 304 angstrom, while the long-lived stable filaments display dark morphology as in 211 angstrom. This suggests that the plasma around 0.5 MK would be an essential component of new-formed filaments and the material temperature in filaments would be variable during their evolution. The filament formed by the recombination of two filaments and an emerged hot loop finally erupts. After reconnection, the final filament shows a highly twisted structure of both bright and dark strands, which is surrounded by several weak and dispersive looplike structures. This eruptive filament has a complex multichannel topology and covers a wide range of temperatures.
学科主题天文学
URL标识查看原文
出版地TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
WOS关键词MAGNETIC RECONNECTION ; SOLAR FILAMENT ; MULTIWAVELENGTH OBSERVATIONS ; ERUPTION ; PROMINENCE ; EVOLUTION ; DRIVEN ; JETS ; FLOWS ; FIELD
资助项目MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166; Precision Mechanics of CAS; Innovation Academy for Microsatellites of CAS[2022YFF0503800]; Innovation Academy for Microsatellites of CAS[2021YFA1600501]; Innovation Academy for Microsatellites of CAS[2021YFA1600503]; Innovation Academy for Microsatellites of CAS[2022YFF0503001]; National Key R&D Program of China[12173050]; National Key R&D Program of China[11973057]; National Key R&D Program of China[12003048]; National Key R&D Program of China[12003051]; National Key R&D Program of China[12173049]; National Key R&D Program of China[11973056]; National Key R&D Program of China[12073040]; National Key R&D Program of China[12073042]; National Key R&D Program of China[12073077]; National Key R&D Program of China[12373115]; National Natural Science Foundations of China
WOS研究方向Astronomy & Astrophysics
语种英语
出版者IOP Publishing Ltd
WOS记录号WOS:001110278500001
资助机构MOST divided by National Key Research and Development Program of China (NKPs)https://doi.org/10.13039/501100012166 ; Precision Mechanics of CAS ; Innovation Academy for Microsatellites of CAS[2022YFF0503800, 2021YFA1600501, 2021YFA1600503, 2022YFF0503001] ; National Key R&D Program of China[12173050, 11973057, 12003048, 12003051, 12173049, 11973056, 12073040, 12073042, 12073077, 12373115] ; National Natural Science Foundations of China
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/26486]  
专题天文技术实验室
作者单位1.Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People's Republic of China;
2.University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China;
3.School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China;
4.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, People's Republic of China
5.National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100101, People's Republic of China;
推荐引用方式
GB/T 7714		 Huang, Jing,Zhang, Yin,Tan, Baolin,et al. Formation and Dynamics in an Observed Preeruptive Filament[J]. ASTROPHYSICAL JOURNAL LETTERS,2023,958(1).
APA Huang, Jing.,Zhang, Yin.,Tan, Baolin.,Bai, Xianyong.,Li, Leping.,...&Deng, Yuanyong.(2023).Formation and Dynamics in an Observed Preeruptive Filament.ASTROPHYSICAL JOURNAL LETTERS,958(1).
MLA Huang, Jing,et al."Formation and Dynamics in an Observed Preeruptive Filament".ASTROPHYSICAL JOURNAL LETTERS 958.1(2023).

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