Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption
We investigate the complex magnetic reconnection process between the filament and surrounding loops during the failed filament eruption that occurred in NOAA active region 13445 on 2023 September 24, using extreme-ultraviolet observations from the Solar Dynamics Observatory and high-resolution H α i...
Saved in:
| Main Authors: | , , , , , , , , , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/addec9 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1849321082046119936 |
|---|---|
| author | Yudi Ou Yingna Su Qingmin Zhang Haisheng Ji Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Zhe Xu Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu |
| author_facet | Yudi Ou Yingna Su Qingmin Zhang Haisheng Ji Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Zhe Xu Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu |
| author_sort | Yudi Ou |
| collection | DOAJ |
| description | We investigate the complex magnetic reconnection process between the filament and surrounding loops during the failed filament eruption that occurred in NOAA active region 13445 on 2023 September 24, using extreme-ultraviolet observations from the Solar Dynamics Observatory and high-resolution H α imaging from the New Vacuum Solar Telescope. This failed filament eruption is associated with an M4.4 flare (SOL2023-09-24T03:28). At the early phase of the filament eruption, the filament displays a distinct clockwise rotational motion, suggesting an untwisting motion. During the flare precursor phase, the northwest slipping motion of the brightenings at the filament’s left footpoint, along with the brightening and continuous expansion of the nearby loops at the northwest, suggest the occurrence of a slipping magnetic reconnection between the filament and peripheral loops at the quasi-separatrix layer. After the slipping motion begins, significant brightenings of filament materials and multiple bright structures moving toward the two filament footpoints are observed during the two episodes of magnetic reconnection between the filament and the overlying loops, with the most prominent brightenings and the moving structures occurring during the main phase of the M4.4 flare. The observed untwisting motion of the filament and the twist reduction derived from the nonlinear force-free field extrapolation suggest that the magnetic reconnection between the filament and the peripheral and overlying loops plays a significant role in the failure of the filament eruption by greatly reducing its twist. |
| format | Article |
| id | doaj-art-96fe93cef5df4a06a4a622084d0f0a2d |
| 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-96fe93cef5df4a06a4a622084d0f0a2d2025-08-20T03:49:50ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198811410.3847/1538-4357/addec9Two Events with Spectacular Moving Structures in a Failed Solar Filament EruptionYudi Ou0https://orcid.org/0009-0005-2677-7998Yingna Su1https://orcid.org/0000-0001-9647-2149Qingmin Zhang2https://orcid.org/0000-0003-4078-2265Haisheng Ji3https://orcid.org/0000-0002-5898-2284Leping Li4https://orcid.org/0000-0001-5776-056XHongqiang Song5https://orcid.org/0000-0001-5705-661XYijun Hou6https://orcid.org/0000-0002-9534-1638Guiping Zhou7https://orcid.org/0000-0001-8228-565XBaolin Tan8https://orcid.org/0000-0003-2047-9664Kaifan Ji9https://orcid.org/0000-0001-8950-3875Zhe Xu10https://orcid.org/0000-0002-9121-9686Yongyuan Xiang11https://orcid.org/0000-0002-5261-6523Zhenyong Hou12https://orcid.org/0000-0003-4804-5673Yang Guo13https://orcid.org/0000-0002-9293-8439Ye Qiu14https://orcid.org/0000-0002-1190-0173Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of China ; ynsu@pmo.ac.cn; 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 ; ynsu@pmo.ac.cn; 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 ; ynsu@pmo.ac.cn; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, 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 ; ynsu@pmo.ac.cn; School of Astronomy and Space Science, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaShandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University , Weihai, Shandong 264209, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People’s Republic of China; University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaKey Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, 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 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 ChinaWe investigate the complex magnetic reconnection process between the filament and surrounding loops during the failed filament eruption that occurred in NOAA active region 13445 on 2023 September 24, using extreme-ultraviolet observations from the Solar Dynamics Observatory and high-resolution H α imaging from the New Vacuum Solar Telescope. This failed filament eruption is associated with an M4.4 flare (SOL2023-09-24T03:28). At the early phase of the filament eruption, the filament displays a distinct clockwise rotational motion, suggesting an untwisting motion. During the flare precursor phase, the northwest slipping motion of the brightenings at the filament’s left footpoint, along with the brightening and continuous expansion of the nearby loops at the northwest, suggest the occurrence of a slipping magnetic reconnection between the filament and peripheral loops at the quasi-separatrix layer. After the slipping motion begins, significant brightenings of filament materials and multiple bright structures moving toward the two filament footpoints are observed during the two episodes of magnetic reconnection between the filament and the overlying loops, with the most prominent brightenings and the moving structures occurring during the main phase of the M4.4 flare. The observed untwisting motion of the filament and the twist reduction derived from the nonlinear force-free field extrapolation suggest that the magnetic reconnection between the filament and the peripheral and overlying loops plays a significant role in the failure of the filament eruption by greatly reducing its twist.https://doi.org/10.3847/1538-4357/addec9Solar filament eruptionsSolar filamentsSolar active region magnetic fieldsSolar active region filamentsSolar magnetic reconnectionSolar activity |
| spellingShingle | Yudi Ou Yingna Su Qingmin Zhang Haisheng Ji Leping Li Hongqiang Song Yijun Hou Guiping Zhou Baolin Tan Kaifan Ji Zhe Xu Yongyuan Xiang Zhenyong Hou Yang Guo Ye Qiu Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption The Astrophysical Journal Solar filament eruptions Solar filaments Solar active region magnetic fields Solar active region filaments Solar magnetic reconnection Solar activity |
| title | Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption |
| title_full | Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption |
| title_fullStr | Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption |
| title_full_unstemmed | Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption |
| title_short | Two Events with Spectacular Moving Structures in a Failed Solar Filament Eruption |
| title_sort | two events with spectacular moving structures in a failed solar filament eruption |
| topic | Solar filament eruptions Solar filaments Solar active region magnetic fields Solar active region filaments Solar magnetic reconnection Solar activity |
| url | https://doi.org/10.3847/1538-4357/addec9 |
| work_keys_str_mv | AT yudiou twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT yingnasu twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT qingminzhang twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT haishengji twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT lepingli twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT hongqiangsong twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT yijunhou twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT guipingzhou twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT baolintan twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT kaifanji twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT zhexu twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT yongyuanxiang twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT zhenyonghou twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT yangguo twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption AT yeqiu twoeventswithspectacularmovingstructuresinafailedsolarfilamenteruption |