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Latitude migration of solar filaments
Li KJ(李可军)1,2; Li, KJ (reprint author), CAS, Natl Astron Observ Yunnan Observ, Kunming 650011, Peoples R China.
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2010-06-21
Volume405Issue:2Pages:1040-1046
DOI10.1111/j.1365-2966.2010.16508.x
Contribution Rank第1完成单位
Indexed BySCI
KeywordMethods: Data Analysis Sun: Activity Sun: Filaments Prominences
AbstractThe Carte Synoptique catalogue of solar filaments from 1919 March-1989 December, corresponding to complete cycles 16-21, is utilized to show the latitudinal migration of filaments at low latitudes (less than 50 degrees), and the latitudinal drift of solar filaments in each hemisphere in each cycle of the time interval is compared with the corresponding drift of sunspot groups. The latitudinal drift of filaments obviously differs from that of sunspot groups. At the beginning of a cycle, filaments (sunspot groups) migrate from latitudes of about 40 degrees (28 degrees) with a drift velocity of about 2.4 m s-1 (1.2 m s-1) toward the solar equator, reach latitudes of about 25 degrees (20 degrees) 4 yr later at the cycle maximum with a drift velocity of about 1.0 m s-1 (1.0 m s-1) and halt at about 8 degrees (8 degrees) at the end of the cycle. When solar activity is programmed into a solar cycle, the difference between the latitudes of appearance of filaments and sunspot groups becomes smaller and smaller. The difference rapidly decreases in the first and last similar to 4 yr of a cycle, but barely decreases at all in the similar to 4 yr after the cycle maximum. For filaments, the latitudinal drift velocity decreases in the first similar to 7.5 yr of a cycle, but increases in the last similar to 3.5 yr of the cycle. However, for sunspot groups the drift velocity always decreases over the whole cycle. The difference between the latitude drift of filaments in the northern and southern hemispheres is found not to be obvious. The latitudinal drift velocity of filaments differs slightly in the northern and southern hemispheres within a cycle. The physical implication behind the latitudinal drift of filaments is explored.
Funding OrganizationNSFC [10583032, 10921303, 40636031] ; National Key Research Science Foundation [2006CB806303] ; Chinese Academy of Sciences
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN0035-8711
URL查看原文
Archive Date2010-06-25
WOS IDWOS:000278677800023
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordACTIVITY CYCLE ; MERIDIONAL FLOW ; SUNSPOT GROUPS ; GREEN CORONA ; PROMINENCES ; DYNAMO ; PERIOD ; MODEL ; SUN
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Cited Times:19[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6166
Collection太阳物理研究组
Corresponding AuthorLi, KJ (reprint author), CAS, Natl Astron Observ Yunnan Observ, Kunming 650011, Peoples R China.
Affiliation1.National Astronomical Observatories/Yunnan Observatory, CAS, Kunming 650011, China
2.Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, China
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Li KJ,Li, KJ . Latitude migration of solar filaments[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2010,405(2):1040-1046.
APA Li KJ,&Li, KJ .(2010).Latitude migration of solar filaments.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,405(2),1040-1046.
MLA Li KJ,et al."Latitude migration of solar filaments".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 405.2(2010):1040-1046.
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