Modeling of the distribution of polarization in the coronal green line on July 11, 1991

Details Modeling of the distribution of polarization in the coronal green line on July 11, 1991 Modeling of the distribution of polarization in the coronal green line on July 11, 1991

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..191b&link_type=abstract

Astronomy Reports, Volume 43, Issue 3, March 1999, pp.191-197

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Model calculations describing the distribution of the polarization of the FeXIV lambda 5303 Angstrom coronal green line observed on July 11, 1991, are presented. The observed properties of the polarization distribution include the presence of an anti-correlation between the degree of polarization p and the intensity I_lambda, and differences in this relation and its dependence on distance for equatorial regions and high-latitude streamers. Grids of uniform models were computed for combinations of two total rates of excitation of the upper line level by electron collisions and two relative abundances for the FeXIV ions. For each combination of parameters, there is a limiting degree of polarization for a given intensity. Description of all the observed values of p and I_lambda requires a wide range of models: the presence of small p and large I_lambda requires models with large densities at the base of the corona n_0 > 1.5 x 10^9 cm^-3; large p with small I_lambda requires models with n_0 < 2 x 10^8 cm^-3. Investigation of inhomogeneous models indicates that the polarization is primarily determined by the characteristic ("mean") density along the line of sight, and not by the presence of structure in the corona. These model calculations are not able to explain the existence of the observed zone absent of points on the p-I_lambda diagram, and some other properties. The influence of coronal magnetic fields on the green-line scattering matrix is briefly discussed.

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