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第23和24太阳活动周的冕洞与开放磁通量

Coronal Holes and Open Magnetic Flux over Cycles 23 and 24.

作者信息

Lowder Chris, Qiu Jiong, Leamon Robert

机构信息

1Department of Mathematical Sciences, Durham University, Durham, DH1 3LE UK.

2Department of Physics, Montana State University, Bozeman, MT 59717 USA.

出版信息

Sol Phys. 2017;292(1):18. doi: 10.1007/s11207-016-1041-8. Epub 2016 Dec 27.

DOI:10.1007/s11207-016-1041-8
PMID:32355367
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC7175679/
Abstract

As the observational signature of the footprints of solar magnetic field lines open into the heliosphere, coronal holes provide a critical measure of the structure and evolution of these lines. Using a combination of (SOHO/EIT), (SDO/AIA), and (STEREO/EUVI A/B) extreme ultraviolet (EUV) observations spanning 1996 - 2015 (nearly two solar cycles), coronal holes are automatically detected and characterized. Coronal hole area distributions show distinct behavior in latitude, defining the domain of polar and low-latitude coronal holes. The northern and southern polar regions show a clear asymmetry, with a lag between hemispheres in the appearance and disappearance of polar coronal holes.

摘要

作为太阳磁场线足迹进入日球层的观测特征，冕洞提供了这些磁力线结构和演化的关键度量。利用1996年至2015年（近两个太阳周期）期间（太阳和日球层观测台/极紫外成像望远镜）、（太阳动力学天文台/大气成像组件）和（日地关系天文台/极紫外成像仪A/B）的极紫外（EUV）观测数据组合，自动检测并表征冕洞。冕洞面积分布在纬度上呈现出不同的特征，界定了极区冕洞和低纬冕洞的范围。南北极区表现出明显的不对称性，极区冕洞的出现和消失在半球之间存在滞后现象。

https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/3c0e3226c7fa/11207_2016_1041_Fig12_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/a95f17f7b0df/11207_2016_1041_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/73fc0a23753d/11207_2016_1041_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/ef6b3b534fc0/11207_2016_1041_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/cea545125c8b/11207_2016_1041_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/61be69c1e1ec/11207_2016_1041_Fig5_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/72045cd0ccbd/11207_2016_1041_Fig6_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/09893de163ce/11207_2016_1041_Fig7_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/f1649dcb5e47/11207_2016_1041_Fig8_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/3ca1a8c23cb8/11207_2016_1041_Fig9_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/21442821f137/11207_2016_1041_Fig10_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/43a74fe976ef/11207_2016_1041_Fig11_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/3c0e3226c7fa/11207_2016_1041_Fig12_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/a95f17f7b0df/11207_2016_1041_Fig1_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/73fc0a23753d/11207_2016_1041_Fig2_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/ef6b3b534fc0/11207_2016_1041_Fig3_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/cea545125c8b/11207_2016_1041_Fig4_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/61be69c1e1ec/11207_2016_1041_Fig5_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/72045cd0ccbd/11207_2016_1041_Fig6_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/09893de163ce/11207_2016_1041_Fig7_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/f1649dcb5e47/11207_2016_1041_Fig8_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/3ca1a8c23cb8/11207_2016_1041_Fig9_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/21442821f137/11207_2016_1041_Fig10_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/43a74fe976ef/11207_2016_1041_Fig11_HTML.jpg
https://cdn.ncbi.nlm.nih.gov/pmc/blobs/07c8/7175679/3c0e3226c7fa/11207_2016_1041_Fig12_HTML.jpg

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本文引用的文献

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Coronal Holes.冕洞
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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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Differential Rotation and Dynamics of the Solar Interior.太阳内部的较差自转与动力学
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