Green-line polarization observations of the solar corona and their interpretation

Details Green-line polarization observations of the solar corona and their interpretation Green-line polarization observations of the solar corona and their interpretation

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..767b&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 767

Astronomy and Astrophysics

Astronomy

6

Solar Corona, Astronomical Polarimetry, Line Spectra, Spaceborne Astronomy, Photosphere, Emission Spectra, Spectrum Analysis, Solar Electrons, X Ray Astronomy

Scientific paper

Polarization observations in the 5303-A Fe XIV line during the eclipse of July 11, 1991 are presented. A new polarization map probing somewhat greater heights in the corona is constructed, and the distribution of polarization position angles is given. Low degrees of polarization p are obtained in the equatorial regions; at low heights, they are consistent with the results of out-of-eclipse observations. The values for p are higher in regions of high-latitude streamers, and increase substantially with distance from the limb. The method used in the analysis made it possible to separate the line emission into two components (associated with excitation due to electron collisions and with resonant scattering of the photospheric radiation), and also to estimate the density and overall extent of the emitting region. The observed values of p are consistent with current notions about the corona if the relative density of the Fe XIV ion is 2 x 10 exp -5 and the rate of excitation by electron collisions is 5 x 10 exp -9 cu cm/s. The possible role of magnetic fields is briefly discussed.

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