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Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations
Liu Y(刘煜)1,2; Liu, Y (reprint author), Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Peoples R China.
Source PublicationANNALES GEOPHYSICAE
2009
Volume27Issue:7Pages:2771-2777
DOI10.5194/angeo-27-2771-2009
Contribution Rank第1完成单位
Indexed BySCI ; EI
KeywordCorona And Transition Region Solar Physics Magnetic Fields Astrophysics And Astronomy
AbstractSpectropolarimetry using IR wavelength of 1075 nm has been proved to be a powerful tool for directly mapping solar coronal magnetic fields including transverse component directions and line-of-sight component intensities. Solar tomography, or stereoscopy based on EUV observations, can supply 3-D information for some magnetic field lines in bright EUV loops. In a previous paper (Liu and Lin, 2008) the locations of the IR emission sources in the 3-D coordinate system were inferred from the comparison between the polarization data and the potential-field-source-surface (PFSS) model, for one of five west limb regions in the corona (Lin et al., 2004). The paper shows that the region with the loop system in the active region over the photospheric area with strong magnetic field intensity is the region with a dominant contribution to the observed Stokes signals. So, the inversion of the measured Stokes parameters could be done assuming that most of the signals come from a relatively thin layer over the area with a large photospheric magnetic field strength. Here, the five limb coronal regions are studied together in order to study the spatial correlation between the bright EUV loop features and the inferred IR emission sources. It is found that, for the coronal regions above the stronger photospheric magnetic fields, the locations of the IR emission sources are closer to or more consistent with the bright EUV loop locations than those above weaker photospheric fields. This result suggests that the structures of the coronal magnetic fields observed at IR and EUV wavelengths may be different when weak magnetic fields present there.
Funding OrganizationNational Natural Science Foundation of China [10843010]
Language英语
Subject AreaAstronomy & Astrophysics ; Geology ; Meteorology & Atmospheric Sciences
SubtypeArticle
ISSN0992-7689
URL查看原文
WOS IDWOS:000268622700014
WOS Research AreaAstronomy & Astrophysics ; Geology ; Meteorology & Atmospheric Sciences
WOS SubjectAstronomy & Astrophysics ; Geosciences, Multidisciplinary ; Meteorology & Atmospheric Sciences
WOS KeywordEMISSION-LINE POLARIZATION ; SPECTRAL-LINES ; SOLAR CORONA ; DENSITY ; VECTOR ; PROBE
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Cited Times:4[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/7173
Collection选址与日冕观测组
Corresponding AuthorLiu, Y (reprint author), Natl Astron Observ, Yunnan Astron Observ, Kunming 650011, Peoples R China.
Affiliation1.Yunnan Astronomical Observatory, National Astronomical Observatories, Kunming 650011, China
2.Institute for Astronomy, University of Hawaii, 34 Ohia Ku Street, Pukalani, HI 96768, USA
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Liu Y,Liu, Y . Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations[J]. ANNALES GEOPHYSICAE,2009,27(7):2771-2777.
APA Liu Y,&Liu, Y .(2009).Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations.ANNALES GEOPHYSICAE,27(7),2771-2777.
MLA Liu Y,et al."Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations".ANNALES GEOPHYSICAE 27.7(2009):2771-2777.
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