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Coronal magnetic fields from the inversion of linear polarization measurements
Liu, Yu; Lin, Haosheng; Kuhn, Jeff
AA(National Astronomical Observatoires, Yunnan Astronomical Observatory, Kunming 650011, China ; Institute for Astronomy, University of Hawaii, Ohia Ku Street, Pukalani, HI 96768, USA ), AB(Institute for Astronomy, University of Hawaii, Ohia Ku Street, Pukalani, HI 96768, USA), AC(Institute for Astronomy, University of Hawaii, Ohia Ku Street, Pukalani, HI 96768, USA)
Solar and Stellar Variability: Impact on Earth and Planets, Proceedings of the International Astronomical Union, IAU Symposium, Volume 264, p. 96-98
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Sun: corona, Sun: magnetic fields, Sun: infrared
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Real 3-D coronal magnetic field reconstruction is expected to be made based on the technologies of IR spectrometry and tomography, in which the data from other wavelengths can be used as critical reference. Our recent studies focused on this issue are briefly reviewed in this paper. Liu & Lin (2008) first evaluated the validity of potential field source surface model applied to one of five limb regions in the corona by comparing the theoretical polarization maps with SOLARC observations in the IR Fe XIII 10747 Å forbidden coronal emission line (CEL). The five limb coronal regions were then studied together in order to study the spatial relation between the bright EUV features on the solar disk and the inferred IR emission sources, which were obtained from the inversion of the SOLARC linear polarization (LP) measurements (Liu 2009). The inversion for each fiber data in the field of view was made by finding the best location where the difference between the synthesized and the observed polarizations reaches the minimum in the integration path along the line of sight. We found a close relationship between the inferred IR emission source locations and the EUV strong emission positions.

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