Study on the relation of the solar coronal rotation with magnetic field structures
Abstract Daily solar spectral irradiances (SSIs) at the spectral intervals 1–40, 116–264 and 950–1600 nm and four categories of solar small-scale magnetic elements ( $$MF_{no}$$ M F no , $$MF_{anti}$$ M F anti , $$MF_{tran}$$ M F tran and $$MF_{in}$$ M F in ) are used to study the temporal variation...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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Nature Portfolio
2023-11-01
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| Series: | Scientific Reports |
| Online Access: | https://doi.org/10.1038/s41598-023-48447-0 |
| _version_ | 1797415556451663872 |
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| author | N. B. Xiang X. H. Zhao L. H. Deng F. Y. Li S. Zheng |
| author_facet | N. B. Xiang X. H. Zhao L. H. Deng F. Y. Li S. Zheng |
| author_sort | N. B. Xiang |
| collection | DOAJ |
| description | Abstract Daily solar spectral irradiances (SSIs) at the spectral intervals 1–40, 116–264 and 950–1600 nm and four categories of solar small-scale magnetic elements ( $$MF_{no}$$ M F no , $$MF_{anti}$$ M F anti , $$MF_{tran}$$ M F tran and $$MF_{in}$$ M F in ) are used to study the temporal variation of coronal rotation and investigate the relation of the coronal rotation with magnetic field structures through continuous wavelet transform and Pearson correlation analysis. The results reveal the contributions of different magnetic structures to the temporal variation of the rotation for the coronal atmosphere during different phases of the solar cycle. During the solar maximum, the temporal variation of rotation for the coronal plasma atmosphere is mainly dominated by the small-scale magnetic elements of $$MF_{anti}$$ M F anti ; whereas during the epochs of the relatively weak solar activity, it is controlled by the joint effect of the small-scale magnetic elements of both $$MF_{anti}$$ M F anti and $$MF_{in}$$ M F in . The weaker the solar activity, the stronger the effect of $$MF_{in}$$ M F in would be. Furthermore, this study presents an explanation for the inconsistent results for the coronal rotation issue among the previous studies, and also reveals the reason why the coronal atmosphere rotates faster than the lower photosphere. |
| first_indexed | 2024-03-09T05:49:16Z |
| format | Article |
| id | doaj.art-957e2cec92cc485bb7e4c1429592a236 |
| institution | Directory Open Access Journal |
| issn | 2045-2322 |
| language | English |
| last_indexed | 2024-03-09T05:49:16Z |
| publishDate | 2023-11-01 |
| publisher | Nature Portfolio |
| record_format | Article |
| series | Scientific Reports |
| spelling | doaj.art-957e2cec92cc485bb7e4c1429592a2362023-12-03T12:18:15ZengNature PortfolioScientific Reports2045-23222023-11-0113111610.1038/s41598-023-48447-0Study on the relation of the solar coronal rotation with magnetic field structuresN. B. Xiang0X. H. Zhao1L. H. Deng2F. Y. Li3S. Zheng4Yunnan Observatories, Chinese Academy of SciencesState Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of SciencesSchool of Mathematics and Computer Science, Yunnan Minzu UniversityState Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of SciencesCollege of Science, China Three Gorges UniversityAbstract Daily solar spectral irradiances (SSIs) at the spectral intervals 1–40, 116–264 and 950–1600 nm and four categories of solar small-scale magnetic elements ( $$MF_{no}$$ M F no , $$MF_{anti}$$ M F anti , $$MF_{tran}$$ M F tran and $$MF_{in}$$ M F in ) are used to study the temporal variation of coronal rotation and investigate the relation of the coronal rotation with magnetic field structures through continuous wavelet transform and Pearson correlation analysis. The results reveal the contributions of different magnetic structures to the temporal variation of the rotation for the coronal atmosphere during different phases of the solar cycle. During the solar maximum, the temporal variation of rotation for the coronal plasma atmosphere is mainly dominated by the small-scale magnetic elements of $$MF_{anti}$$ M F anti ; whereas during the epochs of the relatively weak solar activity, it is controlled by the joint effect of the small-scale magnetic elements of both $$MF_{anti}$$ M F anti and $$MF_{in}$$ M F in . The weaker the solar activity, the stronger the effect of $$MF_{in}$$ M F in would be. Furthermore, this study presents an explanation for the inconsistent results for the coronal rotation issue among the previous studies, and also reveals the reason why the coronal atmosphere rotates faster than the lower photosphere.https://doi.org/10.1038/s41598-023-48447-0 |
| spellingShingle | N. B. Xiang X. H. Zhao L. H. Deng F. Y. Li S. Zheng Study on the relation of the solar coronal rotation with magnetic field structures Scientific Reports |
| title | Study on the relation of the solar coronal rotation with magnetic field structures |
| title_full | Study on the relation of the solar coronal rotation with magnetic field structures |
| title_fullStr | Study on the relation of the solar coronal rotation with magnetic field structures |
| title_full_unstemmed | Study on the relation of the solar coronal rotation with magnetic field structures |
| title_short | Study on the relation of the solar coronal rotation with magnetic field structures |
| title_sort | study on the relation of the solar coronal rotation with magnetic field structures |
| url | https://doi.org/10.1038/s41598-023-48447-0 |
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