Negative-energy Waves in the Vertical Threads of a Solar Prominence
Solar prominences, intricate structures on the Sun’s limb, have been a subject of fascination owing to their threadlike features and dynamic behaviors. Utilizing data from the New Vacuum Solar Telescope, Chinese H α Solar Explorer, and Solar Dynamics Observatory, this study investigates the transver...
| 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/ad3af8 |
| _version_ | 1797201408040108032 |
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| author | Jincheng Wang Dong Li Chuan Li Yijun Hou Zhike Xue Zhe Xu Liheng Yang Qiaoling Li |
| author_facet | Jincheng Wang Dong Li Chuan Li Yijun Hou Zhike Xue Zhe Xu Liheng Yang Qiaoling Li |
| author_sort | Jincheng Wang |
| collection | DOAJ |
| description | Solar prominences, intricate structures on the Sun’s limb, have been a subject of fascination owing to their threadlike features and dynamic behaviors. Utilizing data from the New Vacuum Solar Telescope, Chinese H α Solar Explorer, and Solar Dynamics Observatory, this study investigates the transverse swaying motions observed in the vertical threads of a solar prominence during its eruption onset on 2023 May 11. The transverse swaying motions were observed to propagate upward, accompanied by upflowing materials at an inclination of 31° relative to the plane of the sky. These motions displayed small-amplitude oscillations with corrected velocities of around 3–4 km s ^−1 and periods of 13–17 minutes. Over time, the oscillations of swaying motion exhibited an increasing pattern in displacement amplitudes, oscillatory periods, and projected velocity amplitudes. Their phase velocities are estimated to be about 26–34 km s ^−1 . An important finding is that these oscillations’ phase velocities are comparable to the upward flow velocities, measured to be around 30–34 km s ^−1 . We propose that this phenomenon is associated with negative-energy wave instabilities, which require comparable velocities of the waves and flows, as indicated by our findings. This phenomenon may contribute to the instability and observed disruption of the prominence. By using prominence seismology, the Alfvén speed and magnetic field strength of the vertical threads have been estimated to be approximately 21.5 km s ^−1 and 1–3G, respectively. This study reveals the dynamics and magnetic properties of solar prominences, contributing to our understanding of their behavior in the solar atmosphere. |
| first_indexed | 2024-04-24T07:47:04Z |
| format | Article |
| id | doaj.art-af367dfbff2b44e08abf4a43ef97327f |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-04-24T07:47:04Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-af367dfbff2b44e08abf4a43ef97327f2024-04-18T20:09:58ZengIOP PublishingThe Astrophysical Journal Letters2041-82052024-01-019652L2810.3847/2041-8213/ad3af8Negative-energy Waves in the Vertical Threads of a Solar ProminenceJincheng Wang0https://orcid.org/0000-0003-4393-9731Dong Li1https://orcid.org/0000-0002-4538-9350Chuan Li2https://orcid.org/0000-0001-7693-4908Yijun Hou3https://orcid.org/0000-0002-9534-1638Zhike Xue4https://orcid.org/0000-0002-6526-5363Zhe Xu5https://orcid.org/0000-0002-9121-9686Liheng Yang6https://orcid.org/0000-0003-0236-2243Qiaoling Li7https://orcid.org/0000-0003-2045-8994Yunnan Observatories, Chinese Academy of Sciences , Kunming Yunnan 650216, People's Republic of China ; wangjincheng@ynao.ac.cn; Yunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, 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 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 China; Institute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University , Suzhou 215163, People's Republic of ChinaYunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People's Republic of China; National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming Yunnan 650216, People's Republic of China ; wangjincheng@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 Yunnan 650216, People's Republic of China ; wangjincheng@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 Yunnan 650216, People's Republic of China ; wangjincheng@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 ChinaSolar prominences, intricate structures on the Sun’s limb, have been a subject of fascination owing to their threadlike features and dynamic behaviors. Utilizing data from the New Vacuum Solar Telescope, Chinese H α Solar Explorer, and Solar Dynamics Observatory, this study investigates the transverse swaying motions observed in the vertical threads of a solar prominence during its eruption onset on 2023 May 11. The transverse swaying motions were observed to propagate upward, accompanied by upflowing materials at an inclination of 31° relative to the plane of the sky. These motions displayed small-amplitude oscillations with corrected velocities of around 3–4 km s ^−1 and periods of 13–17 minutes. Over time, the oscillations of swaying motion exhibited an increasing pattern in displacement amplitudes, oscillatory periods, and projected velocity amplitudes. Their phase velocities are estimated to be about 26–34 km s ^−1 . An important finding is that these oscillations’ phase velocities are comparable to the upward flow velocities, measured to be around 30–34 km s ^−1 . We propose that this phenomenon is associated with negative-energy wave instabilities, which require comparable velocities of the waves and flows, as indicated by our findings. This phenomenon may contribute to the instability and observed disruption of the prominence. By using prominence seismology, the Alfvén speed and magnetic field strength of the vertical threads have been estimated to be approximately 21.5 km s ^−1 and 1–3G, respectively. This study reveals the dynamics and magnetic properties of solar prominences, contributing to our understanding of their behavior in the solar atmosphere.https://doi.org/10.3847/2041-8213/ad3af8Solar oscillationsSolar prominencesSolar coronal waves |
| spellingShingle | Jincheng Wang Dong Li Chuan Li Yijun Hou Zhike Xue Zhe Xu Liheng Yang Qiaoling Li Negative-energy Waves in the Vertical Threads of a Solar Prominence The Astrophysical Journal Letters Solar oscillations Solar prominences Solar coronal waves |
| title | Negative-energy Waves in the Vertical Threads of a Solar Prominence |
| title_full | Negative-energy Waves in the Vertical Threads of a Solar Prominence |
| title_fullStr | Negative-energy Waves in the Vertical Threads of a Solar Prominence |
| title_full_unstemmed | Negative-energy Waves in the Vertical Threads of a Solar Prominence |
| title_short | Negative-energy Waves in the Vertical Threads of a Solar Prominence |
| title_sort | negative energy waves in the vertical threads of a solar prominence |
| topic | Solar oscillations Solar prominences Solar coronal waves |
| url | https://doi.org/10.3847/2041-8213/ad3af8 |
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