Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases
Magnetic flux rope (MFRs) are the most probable core structure of coronal mass ejections (CMEs). Their footpoints on the photosphere are the only feature for which their magnetic properties can be accurately measured, and to some extent, determine the property of the whole MFR. So far, the magnetic...
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2025-01-01
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| author | Yin Zhang Jing Huang Jihong Liu Shangbin Yang Yunfei Yang Baolin Tan |
| author_facet | Yin Zhang Jing Huang Jihong Liu Shangbin Yang Yunfei Yang Baolin Tan |
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| description | Magnetic flux rope (MFRs) are the most probable core structure of coronal mass ejections (CMEs). Their footpoints on the photosphere are the only feature for which their magnetic properties can be accurately measured, and to some extent, determine the property of the whole MFR. So far, the magnetic properties of footpoints are still a mystery. Y. Zhang et al. presented the dynamic evolution of four MFRs involved in a major eruption. For this special event, the footpoints of the MFRs could be identified by extreme-ultraviolet (EUV) brightening and MFR morphology during the preeruption phase, and by conjunction, EUV dimming during the eruption phase. This is a new effort to identify the footpoints of MFRs during the preeruption phase. This identification discloses that all footpoints originate out of the umbra and penumbra of the sunspots. The footpoint areas and magnetic flux during the preeruption phase are about 10 ^7 km ^2 and around the order of 10 ^19 –10 ^20 Mx, respectively. During the eruption phase, the footpoint area and the magnetic flux are about 10 ^8 km ^2 and around the order of 10 ^20 Mx, respectively. The temporal evolution of the magnetic features around the footpoints disclose that all footpoint pairs belong to nonconjugated opposite polarities. This observational evidence will help us to understand the magnetic nature of MFRs and their associated CMEs. |
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| spelling | doaj-art-4d3ebc55cafd46ce86cbef51e64c097d2025-08-20T02:25:47ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979216510.3847/1538-4357/ada383Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption PhasesYin Zhang0https://orcid.org/0000-0002-0093-0350Jing Huang1https://orcid.org/0000-0001-8250-1535Jihong Liu2https://orcid.org/0000-0002-7733-8128Shangbin Yang3https://orcid.org/0000-0002-2967-4522Yunfei Yang4https://orcid.org/0000-0001-9927-7541Baolin Tan5https://orcid.org/0000-0003-2047-9664CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaCAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaShijiazhuang University , Shijiazhuang 050035, People’s Republic of ChinaCAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaFaculty of Information Engineering and Automation/Yunnan Key Laboratory of Computer Technology Application, Kunming University of Science and Technology , Kunming 650500, People’s Republic of ChinaCAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100012, People’s Republic of China; Key Laboratory of Solar Activity and Space Weather, National Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of China; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaMagnetic flux rope (MFRs) are the most probable core structure of coronal mass ejections (CMEs). Their footpoints on the photosphere are the only feature for which their magnetic properties can be accurately measured, and to some extent, determine the property of the whole MFR. So far, the magnetic properties of footpoints are still a mystery. Y. Zhang et al. presented the dynamic evolution of four MFRs involved in a major eruption. For this special event, the footpoints of the MFRs could be identified by extreme-ultraviolet (EUV) brightening and MFR morphology during the preeruption phase, and by conjunction, EUV dimming during the eruption phase. This is a new effort to identify the footpoints of MFRs during the preeruption phase. This identification discloses that all footpoints originate out of the umbra and penumbra of the sunspots. The footpoint areas and magnetic flux during the preeruption phase are about 10 ^7 km ^2 and around the order of 10 ^19 –10 ^20 Mx, respectively. During the eruption phase, the footpoint area and the magnetic flux are about 10 ^8 km ^2 and around the order of 10 ^20 Mx, respectively. The temporal evolution of the magnetic features around the footpoints disclose that all footpoint pairs belong to nonconjugated opposite polarities. This observational evidence will help us to understand the magnetic nature of MFRs and their associated CMEs.https://doi.org/10.3847/1538-4357/ada383Solar coronaSolar coronal mass ejectionsSolar flaresSolar magnetic fields |
| spellingShingle | Yin Zhang Jing Huang Jihong Liu Shangbin Yang Yunfei Yang Baolin Tan Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases The Astrophysical Journal Solar corona Solar coronal mass ejections Solar flares Solar magnetic fields |
| title | Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases |
| title_full | Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases |
| title_fullStr | Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases |
| title_full_unstemmed | Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases |
| title_short | Dynamic Evolution of Magnetic Flux Ropes in Active Region 11429. II. Magnetic Characteristic of the Footpoints During the Preeruption and Eruption Phases |
| title_sort | dynamic evolution of magnetic flux ropes in active region 11429 ii magnetic characteristic of the footpoints during the preeruption and eruption phases |
| topic | Solar corona Solar coronal mass ejections Solar flares Solar magnetic fields |
| url | https://doi.org/10.3847/1538-4357/ada383 |
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