Light Bridges and Solar Active Region Evolution Processes
The formation mechanism of light bridges (LBs) is strongly related to the dynamic evolution of solar active regions (ARs). To study the relationship between LB formation and AR evolution phases, we employ 109 LB samples from 69 ARs in 2014 using observational data from the Helioseismic and Magnetic...
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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 Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/ad2515 |
| _version_ | 1827324519176470528 |
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| author | Fuyu Li Changhui Rao Xinhua Zhao Yang Guo Xiaoying Gong Yuhao Chen Nanbin Xiang Huaning Wang |
| author_facet | Fuyu Li Changhui Rao Xinhua Zhao Yang Guo Xiaoying Gong Yuhao Chen Nanbin Xiang Huaning Wang |
| author_sort | Fuyu Li |
| collection | DOAJ |
| description | The formation mechanism of light bridges (LBs) is strongly related to the dynamic evolution of solar active regions (ARs). To study the relationship between LB formation and AR evolution phases, we employ 109 LB samples from 69 ARs in 2014 using observational data from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. LBs are well matched with the weak field lanes (WFLs), except those aligned on the polarity inversion line of δ sunspots. For penumbral intrusion (type-A) and umbral-dot emergence (type-C) LBs, the WFLs represent the splitting of magnetic flux systems. The sunspots tend to decay and split into several parts after type-A and type-C LBs are formed. For sunspot/umbra-merging (type-B) LBs, the declining WFLs are caused by collisions of flux systems. The sunspots merged and remained stable after type-B LBs formed. We conclude that type-B LBs are formed by collisions of flux systems, while type-A and type-C LBs are generated by splits. The time differences ( δ T ) between LBs appearing and ARs peaking have an average value of 1.06, −1.60, and 1.82 days for type-A, B, and C LBs, with the standard deviations of 3.27, 2.17, and 1.89, respectively. A positive value of δ T means that the LB appears after the AR peaks, whereas a negative δ T means it appears before the peak. Type-A LBs tend to form in the decaying phase or around the peak time. Type-B LBs are more likely to be formed in the developing phase. Type-C LBs mostly take shape in the decaying phase of ARs. |
| first_indexed | 2024-04-25T02:14:48Z |
| format | Article |
| id | doaj.art-45e7a5dff6f246fdad8d7b69ebd15d3c |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2024-04-25T02:14:48Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-45e7a5dff6f246fdad8d7b69ebd15d3c2024-03-07T10:34:38ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492024-01-0127113410.3847/1538-4365/ad2515Light Bridges and Solar Active Region Evolution ProcessesFuyu Li0https://orcid.org/0000-0002-2569-1632Changhui Rao1https://orcid.org/0000-0001-8571-8502Xinhua Zhao2https://orcid.org/0000-0002-9977-2646Yang Guo3https://orcid.org/0000-0002-9293-8439Xiaoying Gong4Yuhao Chen5https://orcid.org/0000-0002-8077-094XNanbin Xiang6Huaning Wang7National Laboratory on Adaptive Optics , Chengdu 610209, People's Republic of China ; lifuyu@ioe.ac.cn, chrao@ioe.ac.cn; State Key Laboratory of Space Weather , National Space Science Center, Chinese Academy of Sciences, People's Republic of China; Institute of Optics and Electronics, Chinese Academy of Sciences, P.O. Box 350, Chengdu 610209, People's Republic of China; Key Laboratory of Modern Astronomy and Astrophysics of the Ministry of Education, Nanjing University , 210093, People's Republic of ChinaNational Laboratory on Adaptive Optics , Chengdu 610209, People's Republic of China ; lifuyu@ioe.ac.cn, chrao@ioe.ac.cn; Institute of Optics and Electronics, Chinese Academy of Sciences, P.O. Box 350, Chengdu 610209, People's Republic of China; University of Chinese Academy of Science , Beijing, People's Republic of ChinaState Key Laboratory of Space Weather , National Space Science Center, Chinese Academy of Sciences, People's Republic of ChinaKey Laboratory of Modern Astronomy and Astrophysics of the Ministry of Education, Nanjing University , 210093, People's Republic of ChinaNational Laboratory on Adaptive Optics , Chengdu 610209, People's Republic of China ; lifuyu@ioe.ac.cn, chrao@ioe.ac.cn; Institute of Optics and Electronics, Chinese Academy of Sciences, P.O. Box 350, Chengdu 610209, People's Republic of China; University of Chinese Academy of Science , Beijing, People's Republic of ChinaUniversity of Chinese Academy of Science , Beijing, People's Republic of China; Yunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People's Republic of ChinaState Key Laboratory of Space Weather , National Space Science Center, Chinese Academy of Sciences, People's Republic of China; Yunnan Observatories, Chinese Academy of Sciences , Kunming 650011, People's Republic of ChinaNational Laboratory on Adaptive Optics , Chengdu 610209, People's Republic of China ; lifuyu@ioe.ac.cn, chrao@ioe.ac.cn; Faculty of Electrical Engineering and Computer Science, Ningbo University , Ningbo 315000, People's Republic of ChinaThe formation mechanism of light bridges (LBs) is strongly related to the dynamic evolution of solar active regions (ARs). To study the relationship between LB formation and AR evolution phases, we employ 109 LB samples from 69 ARs in 2014 using observational data from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. LBs are well matched with the weak field lanes (WFLs), except those aligned on the polarity inversion line of δ sunspots. For penumbral intrusion (type-A) and umbral-dot emergence (type-C) LBs, the WFLs represent the splitting of magnetic flux systems. The sunspots tend to decay and split into several parts after type-A and type-C LBs are formed. For sunspot/umbra-merging (type-B) LBs, the declining WFLs are caused by collisions of flux systems. The sunspots merged and remained stable after type-B LBs formed. We conclude that type-B LBs are formed by collisions of flux systems, while type-A and type-C LBs are generated by splits. The time differences ( δ T ) between LBs appearing and ARs peaking have an average value of 1.06, −1.60, and 1.82 days for type-A, B, and C LBs, with the standard deviations of 3.27, 2.17, and 1.89, respectively. A positive value of δ T means that the LB appears after the AR peaks, whereas a negative δ T means it appears before the peak. Type-A LBs tend to form in the decaying phase or around the peak time. Type-B LBs are more likely to be formed in the developing phase. Type-C LBs mostly take shape in the decaying phase of ARs.https://doi.org/10.3847/1538-4365/ad2515SunspotsSolar active regions |
| spellingShingle | Fuyu Li Changhui Rao Xinhua Zhao Yang Guo Xiaoying Gong Yuhao Chen Nanbin Xiang Huaning Wang Light Bridges and Solar Active Region Evolution Processes The Astrophysical Journal Supplement Series Sunspots Solar active regions |
| title | Light Bridges and Solar Active Region Evolution Processes |
| title_full | Light Bridges and Solar Active Region Evolution Processes |
| title_fullStr | Light Bridges and Solar Active Region Evolution Processes |
| title_full_unstemmed | Light Bridges and Solar Active Region Evolution Processes |
| title_short | Light Bridges and Solar Active Region Evolution Processes |
| title_sort | light bridges and solar active region evolution processes |
| topic | Sunspots Solar active regions |
| url | https://doi.org/10.3847/1538-4365/ad2515 |
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