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Profiles of self-reversed prominence lines interpreted using a three-layered model for the variations of the source function
Li KJ(李可军); Ding YJ(丁有济); Bai JM(白金明); Zhong SH(钟树华); LI, KJ
发表期刊ASTRONOMICAL JOURNAL
1993-07
卷号106期号:1页码:396-400
DOI10.1086/116649
产权排序第1完成单位
收录类别SCI
摘要It is known that the self-reversal of a prominence line is related to the variation of the source function along the line of sight. In this paper, the variable source function represented by a three-layered model has been used to probe the relation between the changing form of the source function and the self-reversal of the prominence line. It is found that: (1) the source function of self-reversed Ha lines increases from the surface towards the center of the prominence, and the source functions at the center are in theory > 1.0 times those on the boundary of the prominence; (2) when the total optical depth at the line center (taulambda0) is not very thick, the self-reversal cannot appear at the line center, although the source function increases from the surface toward the center of the prominence; and (3) with the increase of taulambda0 and the coefficient of the source function, the profile variations follow this order: shallow self-reversal and then deep self-reversal.
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-6256
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WOS记录号WOS:A1993LJ88200036
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]SOLAR PROMINENCES
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6012
专题太阳物理研究组
通讯作者LI, KJ
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Li KJ,Ding YJ,Bai JM,et al. Profiles of self-reversed prominence lines interpreted using a three-layered model for the variations of the source function[J]. ASTRONOMICAL JOURNAL,1993,106(1):396-400.
APA 李可军,丁有济,白金明,钟树华,&LI, KJ.(1993).Profiles of self-reversed prominence lines interpreted using a three-layered model for the variations of the source function.ASTRONOMICAL JOURNAL,106(1),396-400.
MLA 李可军,et al."Profiles of self-reversed prominence lines interpreted using a three-layered model for the variations of the source function".ASTRONOMICAL JOURNAL 106.1(1993):396-400.
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