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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.
发表期刊CHINESE JOURNAL OF ASTRONOMY AND ASTROPHYSICS
2001-04
卷号1期号:2页码:161-175
DOI10.1088/1009-9271/1/2/161
分类号P182
产权排序第1完成单位
收录类别SCI
关键词Line : Formation Radiative Transfer Sun : Atmosphere Sunspots Sun : Magnetic Fields
摘要The 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.
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN1009-9271
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归档日期2001-06-05
WOS记录号WOS:000172248800007
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]STOKES PROFILE ANALYSIS ; FIELDS
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被引频次:2[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/114a53/6044
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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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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