Comparison of computed fluxes for Fe X and Fe XIV lines with observed values at 1980 eclipse

Details Comparison of computed fluxes for Fe X and Fe XIV lines with observed values at 1980 eclipse Comparison of computed fluxes for Fe X and Fe XIV lines with observed values at 1980 eclipse

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..110..271r&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 110, no. 2, 1987, p. 271-280.

Statistics

Computation

9

Ion Production Rates, Iron, Line Spectra, Radiant Flux Density, Solar Eclipses, Solar Heating, Computational Astrophysics, Solar Corona, Solar Temperature, Stellar Spectrophotometry

Scientific paper

Fluxes have been computed for Fe X (6374 Å) and Fe XIV (5303 Å) lines as a function of solar radii and at various coronal temperatures. The electron density derived from the white light corona during the total solar eclipse of 1980 were used in the computations. Fluxes in adjacent continua have also been computed. The computed ratios of line flux to the square of continuum flux at a coronal temperature of 1.6×106K show a good fit with the observed values for Fe X line. Further, radiative excitation seems to dominate over collisional excitation beyond 1.3 solar radius.

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