The Fe XIII 10747 A and Fe XIV 5303 A coronal emission lines polarization

Details The Fe XIII 10747 A and Fe XIV 5303 A coronal emission lines polarization The Fe XIII 10747 A and Fe XIV 5303 A coronal emission lines polarization

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.220..115a&link_type=abstract

In ESA The Hydromagnetics of the Sun p 115-118 (SEE N85-25091 14-92)

Computer Science

2

Emission Spectra, Iron, Line Spectra, Polarization Characteristics, Solar Corona, Solar Magnetic Field, Solar Spectra, Abundance, Magnetic Field Configurations, Stellar Composition

Scientific paper

The polarization of the Fe XIII 10747 A and Fe XIV 5303 A lines was observed. Polarization direction is found to be mainly radial. The average polarization rate is below standard theoretical models by a factor of 3. It is more consistent with models taking into account depolarization effects due to density inhomogeneities and to magnetic field direction. The existence of a large scale pattern of polarization provides evidence for the existence of a large scale structure in the coronal magnetic field. The emission line polarization brightness provides a method to study the heterogeneity of the plasma and abundance of Fe in the corona. The inferred abundance is at least 0.0000007 relative to hydrogen

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