Analysis of Fe I lines /chi between 0.00 eV. and 2.6 eV/ in the solar spectrum using improved damping constants and accurate oscillator strengths - Test of a solar model atmosphere

Details Analysis of Fe I lines /chi between 0.00 eV. and 2.6 eV/ in the solar spectrum using improved damping constants and accurate oscillator strengths - Test of a solar model atmosphere Analysis of Fe I lines /chi between 0.00 eV. and 2.6 eV/ in the solar spectrum using improved damping constants and accurate oscillator strengths - Test of a solar model atmosphere

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...112..209s&link_type=abstract

Astronomy and Astrophysics, vol. 112, no. 2, Aug. 1982, p. 209-214.

Astronomy and Astrophysics

Astrophysics

111

Abundance, Iron, Solar Atmosphere, Solar Spectra, Spectral Line Width, Atmospheric Turbulence, Atomic Excitations, Atomic Spectra, Damping, Fine Structure, Magnetohydrodynamic Turbulence, Stellar Models

Scientific paper

An analysis is made of the equivalent widths of 26 well defined Fe I lines in the solar spectrum measured at five disk positions and in the radiation from the integrated disk. Damping constants based on the measurement of strong solar lines, and on laboratory experiments, together with oscillator strengths measured at Oxford, are used in the analysis. Iron abundances and microturbulent velocities are determined using an LTE analysis with the Holweger and Müller (HM) solar model atmospheres. For this atmosphere the derived iron abundance varies significantly with excitation potential, with the 2.2 eV lines standing out as anomalous. It seems unlikely that this anomaly arises from an inaccurate temperature structure for the model atmosphere. One purpose of the study is to test the ability of a model atmosphere to account for the Fe I spectrum across the disc. The HM model atmosphere performs well in this respect. It gives a mean abundance with excitation potential of log A =7.63.

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