Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments
To better understand the physical connections in sympathetic solar eruptions, we investigated the interaction between two nearby filaments and their successive partial eruptions in the active region (AR) NOAA 12866 on 2021 September 9 by using data from the Solar Dynamics Observatory and the New Vac...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/aca9d2 |
| _version_ | 1797697187048587264 |
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| author | Liping Yang Xiaoli Yan Zhike Xue Jincheng Wang Liheng Yang Qiaoling Li Zhe Xu Yang Peng Xia Sun Xinsheng Zhang |
| author_facet | Liping Yang Xiaoli Yan Zhike Xue Jincheng Wang Liheng Yang Qiaoling Li Zhe Xu Yang Peng Xia Sun Xinsheng Zhang |
| author_sort | Liping Yang |
| collection | DOAJ |
| description | To better understand the physical connections in sympathetic solar eruptions, we investigated the interaction between two nearby filaments and their successive partial eruptions in the active region (AR) NOAA 12866 on 2021 September 9 by using data from the Solar Dynamics Observatory and the New Vacuum Solar Telescope. Based on H α and extreme ultraviolet observations, we found that the right part of one filament (F1) became active first and experienced an obvious rolling motion. Then the whole body of the filament became wider and expanded toward another filament (F2). They collided with each other, and the interaction between them was accompanied by the brightening and bidirectional flows that appeared between them. This implies that magnetic reconnection occurred between the threads of two filaments. The interaction resulted in a rightward motion of F2 at first, and then its activation, and finally part of it erupted. Furthermore, when the erupted F2 deflected rapidly toward the middle part of F1, the left part of F1 erupted with its overlying magnetic fields pushed by F2. These observational results imply that these successive eruptions within a short time are physically linked, and this was caused by the interaction of the filaments. Nonlinear force-free field extrapolation reveals that the magnetic structure of the filament F1 was composed of several magnetic flux ropes with different twists. These results further advance our understanding of partial filament eruptions and sympathetic solar eruptions. |
| first_indexed | 2024-03-12T03:36:40Z |
| format | Article |
| id | doaj.art-5b5f1d89e0da4a5c8c5c2b4bee0d75b6 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:36:40Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-5b5f1d89e0da4a5c8c5c2b4bee0d75b62023-09-03T13:08:35ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194316210.3847/1538-4357/aca9d2Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby FilamentsLiping Yang0Xiaoli Yan1https://orcid.org/0000-0003-2891-6267Zhike Xue2https://orcid.org/0000-0002-6526-5363Jincheng Wang3https://orcid.org/0000-0003-4393-9731Liheng Yang4https://orcid.org/0000-0003-0236-2243Qiaoling Li5https://orcid.org/0000-0003-2045-8994Zhe Xu6https://orcid.org/0000-0002-9121-9686Yang Peng7Xia Sun8Xinsheng Zhang9Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of ChinaDepartment of Physics, Yunnan University , Kunming 650091, People's Republic of China; Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaYunnan Normal University , Kunming 650500, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of China ; yanxl@ynao.ac.cn; University of Chinese Academy of Sciences , Beijing 100049, People's Republic of ChinaTo better understand the physical connections in sympathetic solar eruptions, we investigated the interaction between two nearby filaments and their successive partial eruptions in the active region (AR) NOAA 12866 on 2021 September 9 by using data from the Solar Dynamics Observatory and the New Vacuum Solar Telescope. Based on H α and extreme ultraviolet observations, we found that the right part of one filament (F1) became active first and experienced an obvious rolling motion. Then the whole body of the filament became wider and expanded toward another filament (F2). They collided with each other, and the interaction between them was accompanied by the brightening and bidirectional flows that appeared between them. This implies that magnetic reconnection occurred between the threads of two filaments. The interaction resulted in a rightward motion of F2 at first, and then its activation, and finally part of it erupted. Furthermore, when the erupted F2 deflected rapidly toward the middle part of F1, the left part of F1 erupted with its overlying magnetic fields pushed by F2. These observational results imply that these successive eruptions within a short time are physically linked, and this was caused by the interaction of the filaments. Nonlinear force-free field extrapolation reveals that the magnetic structure of the filament F1 was composed of several magnetic flux ropes with different twists. These results further advance our understanding of partial filament eruptions and sympathetic solar eruptions.https://doi.org/10.3847/1538-4357/aca9d2Solar filamentsSolar filament eruptionsSolar active regions |
| spellingShingle | Liping Yang Xiaoli Yan Zhike Xue Jincheng Wang Liheng Yang Qiaoling Li Zhe Xu Yang Peng Xia Sun Xinsheng Zhang Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments The Astrophysical Journal Solar filaments Solar filament eruptions Solar active regions |
| title | Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments |
| title_full | Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments |
| title_fullStr | Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments |
| title_full_unstemmed | Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments |
| title_short | Sympathetic Partial Filament Eruptions Caused by the Interaction between Two Nearby Filaments |
| title_sort | sympathetic partial filament eruptions caused by the interaction between two nearby filaments |
| topic | Solar filaments Solar filament eruptions Solar active regions |
| url | https://doi.org/10.3847/1538-4357/aca9d2 |
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