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

doi:10.3847/1538-4357/ad245f

	The Evolution of Photospheric Magnetic Fields at the Footpoints of Reconnected Structures in the Solar Atmosphere
	Ding, Tao 2; Zhang, Jun 2; Fang, Yue 2; Hong JC(洪俊超)1; Bi Y(毕以)1; Xiang YY(向永源)1
刊名	ASTROPHYSICAL JOURNAL
	2024-03-01
卷号	964 期号:1
ISSN号	0004-637X
DOI	10.3847/1538-4357/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
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关键词	ACTIVE-REGION ; SMALL-SCALE ; FILAMENT ; FLARE ; FLUX ; ENERGY ; DRIVEN ; NONPOTENTIALITY ; ERUPTION ; DYNAMICS
WOS研究方向	Astronomy & Astrophysics
语种	英语
出版者	IOP Publishing Ltd
WOS记录号	WOS:001183686000001
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
内容类型	期刊论文
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
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).