Formation of Solar Quiescent Coronal Loops through Magnetic Reconnection in an Emerging Active Region
文献类型：期刊论文
| 作者 | Hou,Zhenyong3; Tian,Hui1,3; Chen,Hechao3; Zhu,Xiaoshuai1 ; Huang,Zhenghua2; Bai,Xianyong1; He,Jiansen3; Song,Yongliang1; Xia,Lidong2
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| 刊名 | The Astrophysical Journal
 |
| 出版日期 | 2021-07-01 |
| 卷号 | 915期号:1 |
| 关键词 | Solar coronal loops Solar magnetic reconnection Solar physics Solar active regions Solar magnetic flux emergence |
| ISSN号 | 0004-637X |
| DOI | 10.3847/1538-4357/abff60 |
| 英文摘要 | Abstract Coronal loops are the building blocks of solar active regions. However, their formation mechanism remains poorly understood. Here we present direct observational evidence for the formation of coronal loops through magnetic reconnection as new magnetic fluxes emerge into the solar atmosphere. Extreme-ultraviolet observations by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) clearly show the newly formed loops following magnetic reconnection within a plasma sheet. Formation of the loops is also seen in the Hα line-core images taken by the New Vacuum Solar Telescope. Observations from the Helioseismic and Magnetic Imager on board SDO show that a positive-polarity flux concentration moves toward a negative-polarity one with a speed of ～0.4 km s?1 before the formation of coronal loops. During the loop formation process, we found signatures of flux cancellation and subsequent enhancement of the transverse field between the two polarities. The three-dimensional magnetic field structure reconstructed through a magnetohydrostatic model shows field lines consistent with the loops in AIA images. Numerous bright blobs with an average width of 1.37 Mm appear intermittently in the plasma sheet and move upward with a projected velocity of ～114 km s?1. The temperature, emission measure, and density of these blobs are about 3 MK, 2.0 × 1028 cm?5, and 1.2 × 1010 cm?3, respectively. A power spectral analysis of these blobs indicates that the observed reconnection is likely not dominated by a turbulent process. We have also identified flows with a velocity of 20–50 km s?1 toward the footpoints of the newly formed coronal loops. |
| 语种 | 英语 |
| WOS记录号 | IOP:0004-637X-915-1-ABFF60 |
| 出版者 | The American Astronomical Society |
| 源URL | [http://ir.bao.ac.cn/handle/114a11/56743]  |
| 专题 | 中国科学院国家天文台 |
| 通讯作者 | Tian,Hui |
| 作者单位 | 1.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, People's Republic of China 2.Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, Institute of Space Sciences, Shandong University, Weihai, 264209 Shandong, People's Republic of China 3.School of Earth and Space Sciences, Peking University, Beijing 100871, People's Republic of China; huitian@pku.edu.cn |
| 推荐引用方式 GB/T 7714 | Hou,Zhenyong,Tian,Hui,Chen,Hechao,et al. Formation of Solar Quiescent Coronal Loops through Magnetic Reconnection in an Emerging Active Region[J]. The Astrophysical Journal,2021,915(1). |
| APA | Hou,Zhenyong.,Tian,Hui.,Chen,Hechao.,Zhu,Xiaoshuai.,Huang,Zhenghua.,...&Xia,Lidong.(2021).Formation of Solar Quiescent Coronal Loops through Magnetic Reconnection in an Emerging Active Region.The Astrophysical Journal,915(1). |
| MLA | Hou,Zhenyong,et al."Formation of Solar Quiescent Coronal Loops through Magnetic Reconnection in an Emerging Active Region".The Astrophysical Journal 915.1(2021). |
入库方式： OAI收割
来源：国家天文台
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