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Coronal Magnetic Fields Inferred from Ir Wavelength and Comparison with Euv Observations : Volume 27, Issue 7 (13/07/2009)

By Liu, Y.

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Book Id: WPLBN0003986504
Format Type: PDF Article :
File Size: Pages 7
Reproduction Date: 2015

Title: Coronal Magnetic Fields Inferred from Ir Wavelength and Comparison with Euv Observations : Volume 27, Issue 7 (13/07/2009)  
Author: Liu, Y.
Volume: Vol. 27, Issue 7
Language: English
Subject: Science, Annales, Geophysicae
Collections: Periodicals: Journal and Magazine Collection, Copernicus GmbH
Publication Date:
Publisher: Copernicus Gmbh, Göttingen, Germany
Member Page: Copernicus Publications


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Liu, Y. (2009). Coronal Magnetic Fields Inferred from Ir Wavelength and Comparison with Euv Observations : Volume 27, Issue 7 (13/07/2009). Retrieved from

Description: Yunnan Astronomical Observatory, National Astronomical Observatories, Kunming 650011, China. Spectropolarimetry 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 \citep{liu08} 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.

Coronal magnetic fields inferred from IR wavelength and comparison with EUV observations

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