Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE
The eruption of solar filaments, also known as prominences appearing off limb, is a common phenomenon in the solar atmosphere. It ejects massive plasma and high-energy particles into interplanetary space, disturbing the solar-terrestrial environment. It is vital to obtain the three-dimensional veloc...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/ad1e4f |
| _version_ | 1797345608977088512 |
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| author | Ye Qiu Chuan Li Yang Guo Zhen Li Mingde Ding Linggao Kong |
| author_facet | Ye Qiu Chuan Li Yang Guo Zhen Li Mingde Ding Linggao Kong |
| author_sort | Ye Qiu |
| collection | DOAJ |
| description | The eruption of solar filaments, also known as prominences appearing off limb, is a common phenomenon in the solar atmosphere. It ejects massive plasma and high-energy particles into interplanetary space, disturbing the solar-terrestrial environment. It is vital to obtain the three-dimensional velocity fields of erupting filaments for space-weather predictions. We derive the three-dimensional kinematics of an off-limb prominence and an on-disk filament, respectively, using the full-disk spectral and imaging data detected by the Chinese H α Solar Explorer (CHASE). It is found that both the prominence and the filament experience a fast semicircle-shaped expansion at first. The prominence keeps propagating outward with an increasing velocity until escaping successfully, with the south leg of the prominence finally moving back to the Sun in a swirling manner. For the filament, the internal plasma falls back to the Sun in a counterclockwise rotation in the late ejection, matching the failed eruption without a coronal mass ejection. During the eruptions, both the prominence and the filament show material splitting along the line-of-sight direction, revealed by the bimodal H α spectral profiles. For the prominence, the splitting begins at the top and gradually spreads to almost the whole prominence with a fast blueshift component and a slow redshift component. The material splitting in the filament is more fragmental. As shown by the present results, the CHASE full-disk spectroscopic observations make it possible to systematically study the three-dimensional kinematics of solar filament eruptions. |
| first_indexed | 2024-03-08T11:21:13Z |
| format | Article |
| id | doaj.art-2d06ef9dafa54002b4afc768139debb6 |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-08T11:21:13Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-2d06ef9dafa54002b4afc768139debb62024-01-26T09:01:39ZengIOP PublishingThe Astrophysical Journal Letters2041-82052024-01-019612L3010.3847/2041-8213/ad1e4fThree-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASEYe Qiu0https://orcid.org/0000-0002-1190-0173Chuan Li1https://orcid.org/0000-0001-7693-4908Yang Guo2https://orcid.org/0000-0002-9293-8439Zhen Li3Mingde Ding4https://orcid.org/0000-0002-4978-4972Linggao Kong5https://orcid.org/0000-0003-1350-9722Institute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University , Suzhou 215163, People's Republic of China ; lic@nju.edu.cnInstitute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University , Suzhou 215163, People's Republic of China ; lic@nju.edu.cn; School of Astronomy and Space Science, Nanjing University , Nanjing 210023, People's Republic of China ; lizhen@nju.edu.cn; Key Laboratory for 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 ; lizhen@nju.edu.cn; Key Laboratory for 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 ; lizhen@nju.edu.cn; Key Laboratory for 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 ; lizhen@nju.edu.cn; Key Laboratory for Modern Astronomy and Astrophysics (Nanjing University) , Ministry of Education, 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 China ; lic@nju.edu.cnThe eruption of solar filaments, also known as prominences appearing off limb, is a common phenomenon in the solar atmosphere. It ejects massive plasma and high-energy particles into interplanetary space, disturbing the solar-terrestrial environment. It is vital to obtain the three-dimensional velocity fields of erupting filaments for space-weather predictions. We derive the three-dimensional kinematics of an off-limb prominence and an on-disk filament, respectively, using the full-disk spectral and imaging data detected by the Chinese H α Solar Explorer (CHASE). It is found that both the prominence and the filament experience a fast semicircle-shaped expansion at first. The prominence keeps propagating outward with an increasing velocity until escaping successfully, with the south leg of the prominence finally moving back to the Sun in a swirling manner. For the filament, the internal plasma falls back to the Sun in a counterclockwise rotation in the late ejection, matching the failed eruption without a coronal mass ejection. During the eruptions, both the prominence and the filament show material splitting along the line-of-sight direction, revealed by the bimodal H α spectral profiles. For the prominence, the splitting begins at the top and gradually spreads to almost the whole prominence with a fast blueshift component and a slow redshift component. The material splitting in the filament is more fragmental. As shown by the present results, the CHASE full-disk spectroscopic observations make it possible to systematically study the three-dimensional kinematics of solar filament eruptions.https://doi.org/10.3847/2041-8213/ad1e4fSolar filamentsSolar filament eruptionsSolar coronal mass ejectionsSpectroscopy |
| spellingShingle | Ye Qiu Chuan Li Yang Guo Zhen Li Mingde Ding Linggao Kong Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE The Astrophysical Journal Letters Solar filaments Solar filament eruptions Solar coronal mass ejections Spectroscopy |
| title | Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE |
| title_full | Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE |
| title_fullStr | Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE |
| title_full_unstemmed | Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE |
| title_short | Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE |
| title_sort | three dimensional velocity fields of the solar filament eruptions detected by chase |
| topic | Solar filaments Solar filament eruptions Solar coronal mass ejections Spectroscopy |
| url | https://doi.org/10.3847/2041-8213/ad1e4f |
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