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太阳日冕旋转与磁场结构关系的研究。

Study on the relation of the solar coronal rotation with magnetic field structures.

作者信息

Xiang N B, Zhao X H, Deng L H, Li F Y, Zheng S

机构信息

Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650011, China.

State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing, 100190, China.

出版信息

Sci Rep. 2023 Nov 30;13(1):21089. doi: 10.1038/s41598-023-48447-0.

DOI:10.1038/s41598-023-48447-0
PMID:38036637
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC10689849/
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 ([Formula: see text], [Formula: see text], [Formula: see text] and [Formula: see text]) 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 [Formula: see text]; 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 [Formula: see text] and [Formula: see text]. The weaker the solar activity, the stronger the effect of [Formula: see text] 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.

摘要

利用光谱区间为1 - 40、116 - 264和950 - 1600纳米的日太阳光谱辐照度（SSIs）以及四类太阳小尺度磁元（[公式：见原文]、[公式：见原文]、[公式：见原文]和[公式：见原文]），通过连续小波变换和皮尔逊相关分析来研究日冕旋转的时间变化，并探讨日冕旋转与磁场结构的关系。结果揭示了在太阳活动周期的不同阶段，不同磁结构对日冕大气旋转时间变化的贡献。在太阳活动极大期，日冕等离子体大气旋转的时间变化主要由[公式：见原文]的小尺度磁元主导；而在太阳活动相对较弱的时期，它由[公式：见原文]和[公式：见原文]的小尺度磁元的共同作用控制。太阳活动越弱，[公式：见原文]的作用越强。此外，本研究对先前研究中日冕旋转问题的不一致结果给出了解释，同时也揭示了日冕大气比下层光球旋转更快的原因。

https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/de6cf4039f43/41598_2023_48447_Fig9_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/135abd2a0dba/41598_2023_48447_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/52d7a2aab598/41598_2023_48447_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/02f9fbf066ce/41598_2023_48447_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/f666194a3361/41598_2023_48447_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/9bcb572ced27/41598_2023_48447_Fig5_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/c5a8508f21ec/41598_2023_48447_Fig6_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/09bab712355e/41598_2023_48447_Fig7_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/2dfd21bd2f2c/41598_2023_48447_Fig8_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/de6cf4039f43/41598_2023_48447_Fig9_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/135abd2a0dba/41598_2023_48447_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/52d7a2aab598/41598_2023_48447_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/02f9fbf066ce/41598_2023_48447_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/f666194a3361/41598_2023_48447_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/9bcb572ced27/41598_2023_48447_Fig5_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/c5a8508f21ec/41598_2023_48447_Fig6_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/09bab712355e/41598_2023_48447_Fig7_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/2dfd21bd2f2c/41598_2023_48447_Fig8_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/37c1/10689849/de6cf4039f43/41598_2023_48447_Fig9_HTML.jpg

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本文引用的文献

1
The role and contribution of magnetic fields, characterized via their magnetic flux, to the statistical structuring of the solar atmosphere.通过磁通量表征的磁场对太阳大气统计结构的作用和贡献。
Sci Rep. 2022 Sep 23;12(1):15877. doi: 10.1038/s41598-022-20094-x.
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Recent advances in coronal heating.日冕加热的最新进展。
Philos Trans A Math Phys Eng Sci. 2015 May 28;373(2042). doi: 10.1098/rsta.2014.0269.
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The solar magnetic activity band interaction and instabilities that shape quasi-periodic variability.塑造准周期变化的太阳磁活动带相互作用和不稳定性。
Nat Commun. 2015 Apr 7;6:6491. doi: 10.1038/ncomms7491.
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Astronomy. Why is the sun's corona so hot?天文学。为什么日冕如此炽热？
Science. 2012 Jun 1;336(6085):1099. doi: 10.1126/science.336.6085.1099.