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Viewing the "rush to the poles" through phase analysis
Kong DF(孔德芳)1,2; Xiang NB(向南彬)1,2; Pan, GM3
Source PublicationPUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
2014-02
Volume66Issue:1Pages:1-8
DOI10.1093/pasj/pst029
Contribution Rank第1完成单位
Indexed BySCI
Keywordmethods: data analysis Sun: activity Sun: filaments, prominences
Abstract

At mid and low heliographic latitudes, filament activity shifts equatorward starting from the beginning of the solar cycle. At high latitudes, it migrates poleward. Solar filaments exhibit the "rush to the poles" close to solar maximum, when the solar polar magnetic field reverses polarity. In order to better understand the behavior of the "rush to the poles," we used cross-correlation analysis and wavelet transform methods for investigating the periodic characteristics and the phase relationship between two groups of the solar filaments at high latitudes observed during the period from 1919 March to 1989 December. The length of the solar cycle derived from the continuous wavelet transform is a function of latitude, but still shows a significant 11-yr cycle. The most significant periods of the solar filaments, respectively at higher latitudes than 50 degrees and 60 degrees, are 10.77 and 10.62 yr, using the wavelet transform method. From the cross-correlation analysis, the solar filaments at higher latitudes than 50 degrees have a lead of six months with respect to those at higher latitudes than 60 degrees. Different solar cycles exhibited different phase relationships between the two groups of solar filaments. The analysis of the cross-wavelet transform also indicates that the solar filaments at higher latitudes than 50 degrees lead those at higher latitudes than 60 degrees in the entire time interval. The relationship between the phase difference of the two groups of solar filaments and the intensity of solar activity is also discussed. What is more, the poleward shifting speeds are estimated.

Funding ProjectNational Natural Science Foundation of China (NSFC)[11273057] ; National Natural Science Foundation of China (NSFC)[11221063] ; National Natural Science Foundation of China (NSFC)[11373066] ; Key Laboratory of Solar Activity of CAS[KLSA201303] ; 973 programs[2012CB957801] ; Key Laboratory of Solar Activity of CAS[KLSA201303] ; 973 programs[2011CB811406]
Funding OrganizationNational Natural Science Foundation of China (NSFC)[11273057, 11221063, 11373066] ; Key Laboratory of Solar Activity of CAS[KLSA201303] ; 973 programs[2012CB957801, 2011CB811406]
Language英语
Subject Area天文学 ; 太阳与太阳系 ; 太阳物理学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherOXFORD UNIV PRESS
Publication PlaceGREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0004-6264
URL查看原文
Archive Date2014-03-18
WOS IDWOS:000339426900029
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordWAVELET TRANSFORM ANALYSES ; LATITUDE SOLAR-ACTIVITY ; CORONAL MASS EJECTIONS ; MAGNETIC-FIELDS ; ACTIVITY CYCLE ; TIME-SERIES ; SUNSPOT ACTIVITY ; MERIDIONAL FLOW ; FLARE ACTIVITY ; FILAMENTS
Citation statistics
Cited Times:6[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6258
Collection太阳物理研究组
Corresponding AuthorKong DF(孔德芳)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China
2.University of Chinese Academy of Sciences, Beijing 100049, China
3.College of Mathematics Physics and Information Engineering, Jiaxing University, Jiaxing 314001, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Kong DF,Xiang NB,Pan, GM. Viewing the "rush to the poles" through phase analysis[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,2014,66(1):1-8.
APA Kong DF,Xiang NB,&Pan, GM.(2014).Viewing the "rush to the poles" through phase analysis.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,66(1),1-8.
MLA Kong DF,et al."Viewing the "rush to the poles" through phase analysis".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 66.1(2014):1-8.
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