The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot
Solar filaments are believed to be a clump of cold plasma accumulated in the magnetic dips. However, the magnetic configuration of filaments and the key factors for their formation remains elusive. In this Letter, we present a detailed study of the formation and eruption of a multifilament system wi...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/ada893 |
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| author | Haitang Li Jinhan Guo Xin Cheng Chang Zhou Xiaoli Yan Jun Chen Yang Guo Jacob Oloketuyi Mingde Ding Yu Liu |
| author_facet | Haitang Li Jinhan Guo Xin Cheng Chang Zhou Xiaoli Yan Jun Chen Yang Guo Jacob Oloketuyi Mingde Ding Yu Liu |
| author_sort | Haitang Li |
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| description | Solar filaments are believed to be a clump of cold plasma accumulated in the magnetic dips. However, the magnetic configuration of filaments and the key factors for their formation remains elusive. In this Letter, we present a detailed study of the formation and eruption of a multifilament system with observations and simulations. Before the filament appeared visible, the chromospheric fibrils gradually gathered together, evolving from a diffuse distribution into threadlike structures that were nearly parallel to the polarity inversion lines. On 2022 March 20, an arch filament first appeared showing high dynamics, and subsequently two reserved S-shaped filaments were visibly observed. These two filament segments further reconnected, forming a long coherent filament and resulting in a double-decker configuration. In addition, continuous converging motion and magnetic flux cancellation were found in the photosphere during the evolution. Simultaneously, more bald patch structures appeared at the polarities' collision position. Through a data-driven numerical simulation, we further reconstructed the coronal magnetic field, which is composed of two twisted magnetic flux ropes (MFRs) with their bottom touching the photosphere, along with a group of sheared arcades forming an X-shaped configuration. These findings suggest that the magnetic configuration of the filament is in a highly dynamic state, evolving from a hybrid to a coherent MFR. Moreover, we propose that the formation and eruption of the multifilament system are closely related to magnetic reconnection taking place on the photosphere and in the lower corona, respectively, both mainly driven by the photospheric converging motion. |
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| id | doaj-art-1766a5a659ad41d0a9ccd4b65178524c |
| institution | Kabale University |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj-art-1766a5a659ad41d0a9ccd4b65178524c2025-01-29T18:09:59ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019792L4610.3847/2041-8213/ada893The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar SunspotHaitang Li0https://orcid.org/0000-0001-6024-8399Jinhan Guo1https://orcid.org/0000-0002-4205-5566Xin Cheng2https://orcid.org/0000-0003-2837-7136Chang Zhou3https://orcid.org/0009-0009-1911-399XXiaoli Yan4https://orcid.org/0000-0003-2891-6267Jun Chen5https://orcid.org/0000-0003-3060-0480Yang Guo6https://orcid.org/0000-0002-9293-8439Jacob Oloketuyi7https://orcid.org/0000-0003-2439-2910Mingde Ding8https://orcid.org/0000-0002-4978-4972Yu Liu9https://orcid.org/0000-0002-7694-2454School of Physical Science and Technology, Southwest Jiaotong University , Chengdu 611756, People’s Republic of China ; lihaitang@swjtu.edu.cn, lyu@swjtu.edu.cnSchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210023, People’s Republic of ChinaSchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210023, People’s Republic of ChinaSchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210023, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of ChinaPurple Mountain Observatory, Chinese Academy of Sciences , Nanjing 210023, People’s Republic of ChinaSchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210023, People’s Republic of ChinaSchool of Physical Science and Technology, Southwest Jiaotong University , Chengdu 611756, People’s Republic of China ; lihaitang@swjtu.edu.cn, lyu@swjtu.edu.cnSchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People’s Republic of China; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, Nanjing 210023, People’s Republic of ChinaSchool of Physical Science and Technology, Southwest Jiaotong University , Chengdu 611756, People’s Republic of China ; lihaitang@swjtu.edu.cn, lyu@swjtu.edu.cnSolar filaments are believed to be a clump of cold plasma accumulated in the magnetic dips. However, the magnetic configuration of filaments and the key factors for their formation remains elusive. In this Letter, we present a detailed study of the formation and eruption of a multifilament system with observations and simulations. Before the filament appeared visible, the chromospheric fibrils gradually gathered together, evolving from a diffuse distribution into threadlike structures that were nearly parallel to the polarity inversion lines. On 2022 March 20, an arch filament first appeared showing high dynamics, and subsequently two reserved S-shaped filaments were visibly observed. These two filament segments further reconnected, forming a long coherent filament and resulting in a double-decker configuration. In addition, continuous converging motion and magnetic flux cancellation were found in the photosphere during the evolution. Simultaneously, more bald patch structures appeared at the polarities' collision position. Through a data-driven numerical simulation, we further reconstructed the coronal magnetic field, which is composed of two twisted magnetic flux ropes (MFRs) with their bottom touching the photosphere, along with a group of sheared arcades forming an X-shaped configuration. These findings suggest that the magnetic configuration of the filament is in a highly dynamic state, evolving from a hybrid to a coherent MFR. Moreover, we propose that the formation and eruption of the multifilament system are closely related to magnetic reconnection taking place on the photosphere and in the lower corona, respectively, both mainly driven by the photospheric converging motion.https://doi.org/10.3847/2041-8213/ada893Solar filamentsSolar magnetic reconnection |
| spellingShingle | Haitang Li Jinhan Guo Xin Cheng Chang Zhou Xiaoli Yan Jun Chen Yang Guo Jacob Oloketuyi Mingde Ding Yu Liu The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot The Astrophysical Journal Letters Solar filaments Solar magnetic reconnection |
| title | The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot |
| title_full | The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot |
| title_fullStr | The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot |
| title_full_unstemmed | The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot |
| title_short | The Formation of a Multifilament System Driven by Photospheric Converging Motions in a Bipolar Sunspot |
| title_sort | formation of a multifilament system driven by photospheric converging motions in a bipolar sunspot |
| topic | Solar filaments Solar magnetic reconnection |
| url | https://doi.org/10.3847/2041-8213/ada893 |
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