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Key properties of solar chromospheric line formation process
Qu ZQ(屈中权)1,2; Xu Z(徐稚)1,2; Qu, ZQ (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
发表期刊CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS
2002-02
卷号2期号:1页码:71-80
DOI10.1088/1009-9271/2/1/71
分类号P144
产权排序第1完成单位
收录类别SCI
关键词Line : Formation Radiative Transfer Sun : Chromosphere
摘要The distribution or wavelength-dependence of the formation regions of frequently used solar lines, Halpha, Hbeta, CaIIH and CaII8542, in quiet Sun, faint and bright flares is explored in the unpolarized case. We stress four aspects characterising the property of line formation process: 1) width of line formation core; 2) line formation region; 3) influence of the temperature minimum region; and 4) wavelength ranges within which one can obtain pure chromospheric and photospheric filtergrams. It is shown that the above four aspects depend strongly on the atmospheric physical condition and the lines used. The formation regions of all the wavelength points within a line may be continuously distributed over one depth domain or discretely distributed because of no contribution coming from the temperature minimum region, an important domain in the solar atmosphere that determines the distribution pattern of escape photons. On the other hand, the formation region of one wavelength point may cover only one height range or spread over two domains which are separated again by the temperature minimum region. Different lines may form in different regions in the quiet Sun. However, these line formation regions become closer in solar flaring regions. Finally, though the stratification of line-of-sight velocity can alter the position of the line formation core within the line band and result in the asymmetry of the line formation core about the shifted line center, it can only lead to negligible changes in the line formation region or the line formation core width. All these results can be instructive to solar filtering observations.
项目资助者Item 199730l6 of National Science Founda-tion of China and National Major Project 973 under the grant G2000078401. The authors
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN1009-9271
URL查看原文
归档日期2002-02-25
WOS记录号WOS:000174082600009
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]MODELS
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被引频次:14[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/6054
专题太阳物理研究组
通讯作者Qu, ZQ (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
作者单位1.Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011
2.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012
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GB/T 7714
Qu ZQ,Xu Z,Qu, ZQ . Key properties of solar chromospheric line formation process[J]. CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS,2002,2(1):71-80.
APA Qu ZQ,Xu Z,&Qu, ZQ .(2002).Key properties of solar chromospheric line formation process.CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS,2(1),71-80.
MLA Qu ZQ,et al."Key properties of solar chromospheric line formation process".CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS 2.1(2002):71-80.
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