Tracking an eruptive prominence using multiwavelength and multiview observations on 2023 March 7
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arXiv
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| Format: | Preprint |
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2024
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| author | Zhang, Qingmin Ou, Yudi Huang, Zhenghua Song, Yongliang Ma, Suli |
| author_facet | Zhang, Qingmin Ou, Yudi Huang, Zhenghua Song, Yongliang Ma, Suli |
| contents | In this paper, we carry out multiwavelength and multiview observations of the prominence eruption, which generates a C2.3 class flare and a coronal mass ejection (CME) on 2023 March 7. For the first time, we apply the revised cone model to three-dimension reconstruction and tracking of the eruptive prominence for ~4 hrs. The prominence propagates non-radially and makes a detour around the large-scale coronal loops in active region NOAA 13243. The northward deflection angle increases from ~36 degrees to ~47 degrees before returning to ~36 degrees and keeping up. There is no longitudinal deflection throughout the propagation. The angular width of the cone increases from ~30 degrees and reaches a plateau at ~37 degrees. The heliocentric distance of the prominence rises from ~1.1 to ~10.0 solar radii, and the prominence experiences continuous acceleration (~51 m/s^2) over two hours, which is probably related to the magnetic reconnection during the C-class flare. The true speed of CME front is estimated to be ~829 km/s, which is ~1.2 times larger than that of CME core (prominence). It is concluded that both acceleration and deflection of eruptive prominences in their early lives could be reproduced with the revised cone model. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_22724 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Tracking an eruptive prominence using multiwavelength and multiview observations on 2023 March 7 Zhang, Qingmin Ou, Yudi Huang, Zhenghua Song, Yongliang Ma, Suli Solar and Stellar Astrophysics In this paper, we carry out multiwavelength and multiview observations of the prominence eruption, which generates a C2.3 class flare and a coronal mass ejection (CME) on 2023 March 7. For the first time, we apply the revised cone model to three-dimension reconstruction and tracking of the eruptive prominence for ~4 hrs. The prominence propagates non-radially and makes a detour around the large-scale coronal loops in active region NOAA 13243. The northward deflection angle increases from ~36 degrees to ~47 degrees before returning to ~36 degrees and keeping up. There is no longitudinal deflection throughout the propagation. The angular width of the cone increases from ~30 degrees and reaches a plateau at ~37 degrees. The heliocentric distance of the prominence rises from ~1.1 to ~10.0 solar radii, and the prominence experiences continuous acceleration (~51 m/s^2) over two hours, which is probably related to the magnetic reconnection during the C-class flare. The true speed of CME front is estimated to be ~829 km/s, which is ~1.2 times larger than that of CME core (prominence). It is concluded that both acceleration and deflection of eruptive prominences in their early lives could be reproduced with the revised cone model. |
| title | Tracking an eruptive prominence using multiwavelength and multiview observations on 2023 March 7 |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2410.22724 |