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The Evolution of Photospheric Magnetic Fields at the Footpoints of Reconnected Structures in the Solar Atmosphere

文献类型：期刊论文

作者Ding, Tao2; Zhang, Jun2; Fang, Yue2; Hong JC(洪俊超)1; Bi Y(毕以)1; Xiang YY(向永源)1
刊名ASTROPHYSICAL JOURNAL
出版日期2024-03-01
卷号964期号:1
ISSN号0004-637X
DOI10.3847/1538-4357/ad245f
产权排序第2完成单位
文献子类Article
英文摘要Magnetic reconnection is believed to play an important role in the release and conversion of energy among magnetized plasma systems. So far, we have been unable to understand under what conditions magnetic reconnection can take place. Based on observations from the New Vacuum Solar Telescope and the Solar Dynamics Observatory (SDO), we study 16 magnetic reconnection events, and each event has a clear X-type configuration consisting of two sets of atmospheric structures. We focus on 38 footpoints that are relevant to these structures and can be clearly determined. By using SDO/Helioseismic and Magnetic Imager line-of-sight magnetograms, we track the field evolution of these footpoints. Prior to the occurrence of magnetic reconnection, the associated fields at the footpoints underwent convergence and shear motions, and thus became enhanced and complex. During the converging period, the rates of increase of the mean magnetic flux densities (MFDs) at these footpoints are 0.03-0.25 hr-1. While the unsigned mean MFDs are 70-300 G, magnetic reconnection in the solar atmosphere takes place. Subsequently, the photospheric fields of these footpoints diffuse and weaken, with rates of decrease of the MFDs from 0.03 to 0.18 hr-1. These results suggest that, due to the photospheric dynamical evolution at the footpoints, the footpoint MFDs increase from a small value to a large one, and the corresponding atmospheric magnetic fields become complicated and nonpotential; then reconnection happens and it releases the accumulated magnetic field energy. Our study supports the conjecture that magnetic reconnection releases free magnetic energy stored in the nonpotential fields.
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ACTIVE-REGION ; SMALL-SCALE ; FILAMENT ; FLARE ; FLUX ; ENERGY ; DRIVEN ; NONPOTENTIALITY ; ERUPTION ; DYNAMICS
资助项目MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[12073001]; MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[12173084]; MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[12273016]; National Natural Science Foundations of China[2021YFA1600500]; National Natural Science Foundations of China[2019YFA0405000]; National Key R&D Programs of China[Z010118169]; Anhui Project
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001183686000001
出版者IOP Publishing Ltd
资助机构MOST divided by National Natural Science Foundation of China (NSFC)https://doi.org/10.13039/501100001809[12073001, 12173084, 12273016] ; National Natural Science Foundations of China[2021YFA1600500, 2019YFA0405000] ; National Key R&D Programs of China[Z010118169] ; Anhui Project
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/26474]  
专题云南天文台_太阳物理研究组
云南天文台_抚仙湖太阳观测站
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, People's Republic of China
2.School of Physics and Optoelectronics Engineering, Anhui University, Hefei 230601, People's Republic of China; zjun@ahu.edu.cn;
推荐引用方式
GB/T 7714		 Ding, Tao,Zhang, Jun,Fang, Yue,et al. The Evolution of Photospheric Magnetic Fields at the Footpoints of Reconnected Structures in the Solar Atmosphere[J]. ASTROPHYSICAL JOURNAL,2024,964(1).
APA Ding, Tao,Zhang, Jun,Fang, Yue,洪俊超,毕以,&向永源.(2024).The Evolution of Photospheric Magnetic Fields at the Footpoints of Reconnected Structures in the Solar Atmosphere.ASTROPHYSICAL JOURNAL,964(1).
MLA Ding, Tao,et al."The Evolution of Photospheric Magnetic Fields at the Footpoints of Reconnected Structures in the Solar Atmosphere".ASTROPHYSICAL JOURNAL 964.1(2024).

入库方式： OAI收割

来源：云南天文台

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