Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun
In this paper, we carry out multiwavelength and multiview observations of the eruption of an intermediate prominence originating from the farside of the Sun on 2023 March 12. The southeast footpoint of the prominence is located in NOAA Active Region 13252. The eruption generates a B7.8 class flare a...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/add328 |
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| author | Qingmin Zhang Wenwei Pan Beili Ying Li Feng Yiliang Li Xiaoli Yan Liheng Yang Ye Qiu Jun Chen Suli Ma |
| author_facet | Qingmin Zhang Wenwei Pan Beili Ying Li Feng Yiliang Li Xiaoli Yan Liheng Yang Ye Qiu Jun Chen Suli Ma |
| author_sort | Qingmin Zhang |
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| description | In this paper, we carry out multiwavelength and multiview observations of the eruption of an intermediate prominence originating from the farside of the Sun on 2023 March 12. The southeast footpoint of the prominence is located in NOAA Active Region 13252. The eruption generates a B7.8 class flare and a partial halo coronal mass ejection (CME). The prominence takes off at 02:00 UT and accelerates for nearly 3 hr. Rotation of the southeast leg of the prominence in the counterclockwise direction is revealed by spectroscopic and imaging observations. The apex of the prominence changes from a smooth loop to a cusp structure during the rising motion, and the northwest leg displays a drift motion after 04:30 UT, implying a writhing motion. Hence, the prominence eruption is most likely triggered by ideal kink instability. For the first time, we apply the Graduated Cylindrical Shell modeling in 3D reconstruction and tracking of the prominence for nearly 2 hr. Both the source region (110°E, 43°N) and northwest footpoint (162°E, 44°N) are located. The edge-on and face-on angular widths of the prominence are ∼6° and ∼86°, respectively. The axis has a tilt angle of ∼70° with the meridian. The heliocentric distance of the prominence leading edge increases from ∼1.26 R _⊙ to ∼2.27 R _⊙ . The true speed of the CME increases from ∼610 to ∼849 km s ^−1 . |
| format | Article |
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| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-8b0eaebbf50a4288a8d79c97baf240b72025-08-20T03:05:53ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01985223710.3847/1538-4357/add328Tracking an Eruptive Intermediate Prominence Originating from the Farside of the SunQingmin Zhang0https://orcid.org/0000-0003-4078-2265Wenwei Pan1Beili Ying2https://orcid.org/0000-0001-8402-9748Li Feng3https://orcid.org/0000-0003-4655-6939Yiliang Li4Xiaoli Yan5https://orcid.org/0000-0003-2891-6267Liheng Yang6https://orcid.org/0000-0003-0236-2243Ye Qiu7https://orcid.org/0000-0002-1190-0173Jun Chen8https://orcid.org/0000-0003-3060-0480Suli Ma9https://orcid.org/0000-0002-5431-6065Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cn; State Key Laboratory of Solar Activity and Space Weather , Beijing 100190, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cn; Department of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cnKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cnKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cn; Department of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaYunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People’s Republic of China; Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of ChinaYunnan Key Laboratory of Solar Physics and Space Science , Kunming 650216, People’s Republic of China; Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of ChinaInstitute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University , Suzhou 215163, People’s Republic of ChinaKey Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory , Nanjing 210023, People’s Republic of China ; zhangqm@pmo.ac.cnState Key Laboratory of Solar Activity and Space Weather , Beijing 100190, People’s Republic of ChinaIn this paper, we carry out multiwavelength and multiview observations of the eruption of an intermediate prominence originating from the farside of the Sun on 2023 March 12. The southeast footpoint of the prominence is located in NOAA Active Region 13252. The eruption generates a B7.8 class flare and a partial halo coronal mass ejection (CME). The prominence takes off at 02:00 UT and accelerates for nearly 3 hr. Rotation of the southeast leg of the prominence in the counterclockwise direction is revealed by spectroscopic and imaging observations. The apex of the prominence changes from a smooth loop to a cusp structure during the rising motion, and the northwest leg displays a drift motion after 04:30 UT, implying a writhing motion. Hence, the prominence eruption is most likely triggered by ideal kink instability. For the first time, we apply the Graduated Cylindrical Shell modeling in 3D reconstruction and tracking of the prominence for nearly 2 hr. Both the source region (110°E, 43°N) and northwest footpoint (162°E, 44°N) are located. The edge-on and face-on angular widths of the prominence are ∼6° and ∼86°, respectively. The axis has a tilt angle of ∼70° with the meridian. The heliocentric distance of the prominence leading edge increases from ∼1.26 R _⊙ to ∼2.27 R _⊙ . The true speed of the CME increases from ∼610 to ∼849 km s ^−1 .https://doi.org/10.3847/1538-4357/add328Solar flaresSolar prominencesSolar coronal mass ejections |
| spellingShingle | Qingmin Zhang Wenwei Pan Beili Ying Li Feng Yiliang Li Xiaoli Yan Liheng Yang Ye Qiu Jun Chen Suli Ma Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun The Astrophysical Journal Solar flares Solar prominences Solar coronal mass ejections |
| title | Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun |
| title_full | Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun |
| title_fullStr | Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun |
| title_full_unstemmed | Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun |
| title_short | Tracking an Eruptive Intermediate Prominence Originating from the Farside of the Sun |
| title_sort | tracking an eruptive intermediate prominence originating from the farside of the sun |
| topic | Solar flares Solar prominences Solar coronal mass ejections |
| url | https://doi.org/10.3847/1538-4357/add328 |
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