Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops
The failure of a filament eruption caused by magnetic reconnection between the erupting filament and the overlying magnetic field has been previously proposed in numerical simulations. It is, however, rarely observed. In this study, we report a reconnection between an erupting filament and its overl...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad9a56 |
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| author | Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu Yingna Su Haisheng Ji Qingmin Zhang Yudi Ou |
| author_facet | Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu Yingna Su Haisheng Ji Qingmin Zhang Yudi Ou |
| author_sort | Leping Li |
| collection | DOAJ |
| description | The failure of a filament eruption caused by magnetic reconnection between the erupting filament and the overlying magnetic field has been previously proposed in numerical simulations. It is, however, rarely observed. In this study, we report a reconnection between an erupting filament and its overlying coronal loops that results in the failure of the filament eruption. On 2023 September 24, a filament was located in active region 13445. It slowly rose, quickly erupted, rapidly decelerated, then finally stopped, with an untwisting motion. As a failed eruption, the event is associated with an M4.4 flare but no coronal mass ejection. During the eruption, the filament became bright, and the overlying loops appeared first in the high-temperature channels. They have average temperatures of ∼12.8 and ∼9.6 MK, respectively, indicating that both of them were heated. Two sets of new loops, separately connecting the filament endpoints and the overlying loop footpoints, then formed. Subsequently, the heated overlying loops were seen sequentially in the low-temperature channels, showing the cooling process, which is also supported by the light curves. Plasmoids formed and propagated bidirectionally along the filament and the overlying loops, indicating the presence of plasmoid instability. These results suggest that reconnection occurs between the erupting filament and the overlying loops. The erupting filament eventually disappeared, with the appearance of more newly formed loops. We propose that the reconnection between the erupting filament and the overlying loops ruins the filament completely, hence resulting in the failed eruption. |
| format | Article |
| id | doaj-art-8d33cf1b6bc744f8afc89a5382b4e68c |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-8d33cf1b6bc744f8afc89a5382b4e68c2025-01-21T10:22:27ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979211310.3847/1538-4357/ad9a56Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal LoopsLeping Li0https://orcid.org/0000-0001-5776-056XHongqiang Song1https://orcid.org/0000-0001-5705-661XYijun Hou2https://orcid.org/0000-0002-9534-1638Guiping Zhou3https://orcid.org/0000-0001-8228-565XBaolin Tan4https://orcid.org/0000-0003-2047-9664Kaifan Ji5https://orcid.org/0000-0001-8950-3875Yongyuan Xiang6https://orcid.org/0000-0002-5261-6523Zhenyong Hou7https://orcid.org/0000-0003-4804-5673Yang Guo8https://orcid.org/0000-0002-9293-8439Ye Qiu9https://orcid.org/0000-0002-1190-0173Yingna Su10https://orcid.org/0000-0001-9647-2149Haisheng Ji11https://orcid.org/0000-0002-5898-2284Qingmin Zhang12https://orcid.org/0000-0003-4078-2265Yudi Ou13https://orcid.org/0009-0005-2677-7998National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; lepingli@nao.cas.cn; Key Laboratory of Solar Activity and Space Weather , National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaSchool of Space Science and Technology, Shandong University , Weihai, Shandong 264209, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; lepingli@nao.cas.cn; Key Laboratory of Solar Activity and Space Weather , National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; lepingli@nao.cas.cn; Key Laboratory of Solar Activity and Space Weather , National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of China ; lepingli@nao.cas.cn; Key Laboratory of Solar Activity and Space Weather , National Space Science Center, Chinese Academy of Sciences, Beijing 100190, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaYunnan Observatories , Chinese Academy of Sciences, Kunming 650216, People’s Republic of ChinaYunnan Observatories , Chinese Academy of Sciences, Kunming 650216, People’s Republic of ChinaSchool of Earth and Space Sciences, Peking University , Beijing 100871, People’s Republic of ChinaSchool of Astronomy and Space Science and Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University , Nanjing 210023, People’s Republic of ChinaInstitute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University , Suzhou 215163, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy , Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy , Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaYunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People’s Republic of China; Key Laboratory of Dark Matter and Space Astronomy , Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy , Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaThe failure of a filament eruption caused by magnetic reconnection between the erupting filament and the overlying magnetic field has been previously proposed in numerical simulations. It is, however, rarely observed. In this study, we report a reconnection between an erupting filament and its overlying coronal loops that results in the failure of the filament eruption. On 2023 September 24, a filament was located in active region 13445. It slowly rose, quickly erupted, rapidly decelerated, then finally stopped, with an untwisting motion. As a failed eruption, the event is associated with an M4.4 flare but no coronal mass ejection. During the eruption, the filament became bright, and the overlying loops appeared first in the high-temperature channels. They have average temperatures of ∼12.8 and ∼9.6 MK, respectively, indicating that both of them were heated. Two sets of new loops, separately connecting the filament endpoints and the overlying loop footpoints, then formed. Subsequently, the heated overlying loops were seen sequentially in the low-temperature channels, showing the cooling process, which is also supported by the light curves. Plasmoids formed and propagated bidirectionally along the filament and the overlying loops, indicating the presence of plasmoid instability. These results suggest that reconnection occurs between the erupting filament and the overlying loops. The erupting filament eventually disappeared, with the appearance of more newly formed loops. We propose that the reconnection between the erupting filament and the overlying loops ruins the filament completely, hence resulting in the failed eruption.https://doi.org/10.3847/1538-4357/ad9a56Solar filament eruptionsSolar extreme ultraviolet emissionSolar coronaPlasma astrophysicsSolar flaresSolar magnetic reconnection |
| spellingShingle | Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu Yingna Su Haisheng Ji Qingmin Zhang Yudi Ou Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops The Astrophysical Journal Solar filament eruptions Solar extreme ultraviolet emission Solar corona Plasma astrophysics Solar flares Solar magnetic reconnection |
| title | Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops |
| title_full | Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops |
| title_fullStr | Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops |
| title_full_unstemmed | Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops |
| title_short | Failure of a Solar Filament Eruption Caused by Magnetic Reconnection with Overlying Coronal Loops |
| title_sort | failure of a solar filament eruption caused by magnetic reconnection with overlying coronal loops |
| topic | Solar filament eruptions Solar extreme ultraviolet emission Solar corona Plasma astrophysics Solar flares Solar magnetic reconnection |
| url | https://doi.org/10.3847/1538-4357/ad9a56 |
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