Coronal Holes and Open Magnetic Flux over Cycles 23 and 24

被引：62
|
作者：
Lowder, Chris [1 ,2 ]
Qiu, Jiong [2 ]
Leamon, Robert [2 ,3 ]
机构：
[1] Univ Durham, Dept Math Sci, Durham DH1 3LE, England
[2] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA
[3] Univ Maryland, Dept Astron, College Pk, MD 20742 USA
来源：
SOLAR PHYSICS | 2017年 / 292卷 / 01期
关键词：
Coronal holes; Magnetic fields; corona; models; Solar cycle; observations; SOLAR-CYCLE; SUNSPOT CYCLE; EVOLUTION; FIELDS; DYNAMICS; ROTATION; IMAGER; MODEL; SUN;
D O I：
10.1007/s11207-016-1041-8
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 Solar and Heliospheric Observatory/Extreme ultraviolet Imaging Telescope (SOHO/EIT), Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA), and Solar Terrestrial Relations Observatory/Extreme Ultraviolet Imager (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.
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页数：23
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