Coronal emission-line polarization from the statistical equilibrium of magnetic sublevels. II - Fe XIV 5303 A

Details Coronal emission-line polarization from the statistical equilibrium of magnetic sublevels. II - Fe XIV 5303 A Coronal emission-line polarization from the statistical equilibrium of magnetic sublevels. II - Fe XIV 5303 A

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...255..753h&link_type=abstract

Astrophysical Journal, Part 1, vol. 255, Apr. 15, 1982, p. 753-763.

Astronomy and Astrophysics

Astrophysics

15

Iron, Linear Polarization, Polarized Light, Solar Corona, Solar Magnetic Field, Solar Spectra, Electron Density (Concentration), Solar Maximum Mission, Temperature Dependence

Scientific paper

Coronal magnetic fields influence the intensity and linear polarization of light scattered by coronal Fe XIV ions. To interpret polarization measurements of Fe XIV 5303 A coronal emission requires a detailed understanding of the dependence of the emitted Stokes vector on coronal magnetic field direction, electron density, and temperature and on height of origin. The required dependence is included in the solutions of statistical equilibrium for the ion which are solved explicitly for 34 magnetic sublevels in both the ground and four excited terms. The full solutions are reduced to equivalent simple analytic forms which clearly show the required dependence on coronal conditions. The analytic forms of the reduced solutions are suitable for routine analysis of 5303 green line polarimetric data obtained at Pic du Midi and from the Solar Maximum Mission Coronagraph/Polarimeter.

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