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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.
Source PublicationCHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS
2002-02
Volume2Issue:1Pages:71-80
DOI10.1088/1009-9271/2/1/71
ClassificationP144
Contribution Rank第1完成单位
Indexed BySCI
KeywordLine : Formation Radiative Transfer Sun : Chromosphere
AbstractThe 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.
Funding OrganizationItem 199730l6 of National Science Founda-tion of China and National Major Project 973 under the grant G2000078401. The authors
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN1009-9271
URL查看原文
Archive Date2002-02-25
WOS IDWOS:000174082600009
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordMODELS
Citation statistics
Cited Times:14[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6054
Collection太阳物理研究组
Corresponding AuthorQu, ZQ (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
Affiliation1.Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011
2.National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
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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