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On the line formation in stellar magnetized atmospheres
Qu ZQ(屈中权)1,2; Zhang XY(张霄宇)1; Xu Z(徐稚)1; Qu, ZQ (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Peoples R China.
Source PublicationCHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS
2001-04
Volume1Issue:2Pages:161-175
DOI10.1088/1009-9271/1/2/161
ClassificationP182
Contribution Rank第1完成单位
Indexed BySCI
KeywordLine : Formation Radiative Transfer Sun : Atmosphere Sunspots Sun : Magnetic Fields
AbstractThe line formation process in stellar magnetized atmospheres is studied by observing the wavelength-dependence of Stokes contribution functions. The influence of magnetic field on the escape line photon distribution and line absorption is obtained by comparing with the null magnetic field case. Two models are adopted. One assumes limited distributions of both the line absorption and magnetic field where a hypothetical magneto-sensitive line is formed. The other is a model atmosphere of sunspot umbra in which Mg I 5172.7 forms. It is found that the magnetic field influences the formation region of Stokes I at wavelengths sufficient close to the Zeeman splitting points +/- Delta lambda (H). The formation regions at wavelengths far away from the Zeeman splitting points generally show a non-magnetic behaviour. Further, if the line core is split by the Zeeman effect, the line formation core introduced in the previous paper disappears. On the other hand, Stokes Q, U, V at each wavelength within the line form in the same layers where both the line absorption and magnetic field are present in the models accepted for the lines used. When the line absorption and magnetic field ubiquitously exist, the formation regions of the pi peaks or valleys of Stokes Q, U and those of sigma of Stokes V generally cover the widest depth range. It is pointed out that such a study is instructive in the explanation of solar polarized filtergrams. It can tell us at each observation point where the received line photons of wavelengths within the bandpass come from and where their polarization states are formed or give us the distributions of these photons as well as their polarization intensities. Thus a three-dimensional image can be constructed for a morphologic study of the observed area from serial filtergrams.
Language英语
Subject AreaAstronomy & Astrophysics
SubtypeArticle
ISSN1009-9271
URL查看原文
Archive Date2001-06-05
WOS IDWOS:000172248800007
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordSTOKES PROFILE ANALYSIS ; FIELDS
Citation statistics
Cited Times:2[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/6044
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,Zhang XY,Xu Z,et al. On the line formation in stellar magnetized atmospheres[J]. CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS,2001,1(2):161-175.
APA Qu ZQ,Zhang XY,Xu Z,&Qu, ZQ .(2001).On the line formation in stellar magnetized atmospheres.CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS,1(2),161-175.
MLA Qu ZQ,et al."On the line formation in stellar magnetized atmospheres".CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS 1.2(2001):161-175.
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