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Magnetic Reconnection between Loops Accelerated By a Nearby Filament Eruption
Li,Leping1,2; Peter,Hardi3; Chitta,Lakshmi Pradeep3; Song,Hongqiang4; Ji,Kaifan5; Xiang,YongYuan5
2021-02-01
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume908Issue:2
AbstractAbstract Magnetic reconnection modulated by nonlocal disturbances in the solar atmosphere has been investigated theoretically, but rarely observed. In this study, employing Hα and extreme ultraviolet (EUV) images and line-of-sight magnetograms, we report the acceleration of reconnection by an adjacent filament eruption. In Hα images, four groups of chromospheric fibrils are observed to form a saddle-like structure. Among them, two groups of fibrils converge and reconnect. Two newly reconnected fibrils then form and retract away from the reconnection region. In EUV images, similar structures and evolution of coronal loops are identified. The current sheet forms repeatedly at the interface of reconnecting loops, with a width and length of 1–2 and 5.3–7.2 Mm and a reconnection rate of 0.18–0.3. It appears in the EUV low-temperature channels, with an average differential emission measure (DEM) weighed temperature and EM of 2 MK and 2.5 × 1027 cm?5. Plasmoids appear in the current sheet and propagate along it, and then further along the reconnection loops. The filament, located to the southeast of the reconnection region, erupts and pushes away the loops covering the reconnection region. Thereafter, the current sheet has a width and length of 2 and 3.5 Mm and a reconnection rate of 0.57. It becomes much brighter and appears in the EUV high-temperature channels, with an average DEM-weighed temperature and EM of 5.5 MK and 1.7 × 1028 cm?5. In the current sheet, more hotter plasmoids form. More thermal and kinetic energy is hence converted. These results suggest that the reconnection is significantly accelerated by the propagating disturbance caused by the nearby filament eruption.
KeywordSolar magnetic reconnection Plasma physics Solar corona Solar ultraviolet emission Solar magnetic fields
DOI10.3847/1538-4357/abd47e
Language英语
WOS IDIOP:0004-637X-908-2-abd47e
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/59695
Collection中国科学院国家天文台
Corresponding AuthorLi,Leping
Affiliation1.CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of China lepingli@nao.cas.cn
2.University of Chinese Academy of Sciences, Beijing 100049, People’s Republic of China
3.Max Planck Institute for Solar System Research, D-37077 G?ttingen, Germany
4.Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209, People’s Republic of China
5.Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, People’s Republic of China
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Li,Leping,Peter,Hardi,Chitta,Lakshmi Pradeep,et al. Magnetic Reconnection between Loops Accelerated By a Nearby Filament Eruption[J]. The Astrophysical Journal,2021,908(2).
APA Li,Leping,Peter,Hardi,Chitta,Lakshmi Pradeep,Song,Hongqiang,Ji,Kaifan,&Xiang,YongYuan.(2021).Magnetic Reconnection between Loops Accelerated By a Nearby Filament Eruption.The Astrophysical Journal,908(2).
MLA Li,Leping,et al."Magnetic Reconnection between Loops Accelerated By a Nearby Filament Eruption".The Astrophysical Journal 908.2(2021).
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