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Diagnostic of spectral lines in magnetized solar atmosphere: Formation of the H β line in sunspots
Zhang Hongqi
2020
Source PublicationScience China. Physics, Mechanics & Astronomy
ISSN1674-7348
Volume63Issue:11
AbstractFormation of the H β λ 4861.34 A line is an important topic related to the diagnosis of the basic configuration of magnetic fields in the solar and stellar chromospheres. Specifically, broadening of the H β λ 4861.34 A line occurs due to the magnetic and microelectric fields in the solar atmosphere. The formation of H β in the model umbral atmosphere is presented based on the assumption of non-local thermodynamic equilibrium. It is found that the model umbral chromosphere is transparent to the Stokes parameters of the H β line, which implies that the observed signals of magnetic fields at sunspot umbrae via the H β line originate from the deep solar atmosphere, where lg τ_c ≈ – 1 (about 300 km in the photospheric layer for our calculations). This is in contrast to the observed Stokes signals from non-sunspot areas, which are thought to primarily form in the solar chromosphere.
Keywordsolar spectrum polarization-Stokes parameters magnetic fields
Language英语
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/73917
Collection中国科学院国家天文台
Affiliation中国科学院国家天文台
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Zhang Hongqi. Diagnostic of spectral lines in magnetized solar atmosphere: Formation of the H β line in sunspots[J]. Science China. Physics, Mechanics & Astronomy,2020,63(11).
APA Zhang Hongqi.(2020).Diagnostic of spectral lines in magnetized solar atmosphere: Formation of the H β line in sunspots.Science China. Physics, Mechanics & Astronomy,63(11).
MLA Zhang Hongqi."Diagnostic of spectral lines in magnetized solar atmosphere: Formation of the H β line in sunspots".Science China. Physics, Mechanics & Astronomy 63.11(2020).
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