Interpretation of the solar spectrum 300-900 nm. II - Fe I lines of excitation potential 0.00-1.01 eV: Use of new oscillator strengths of 0.5 per cent accuracy

Details Interpretation of the solar spectrum 300-900 nm. II - Fe I lines of excitation potential 0.00-1.01 eV: Use of new oscillator strengths of 0.5 per cent accuracy Interpretation of the solar spectrum 300-900 nm. II - Fe I lines of excitation potential 0.00-1.01 eV: Use of new oscillator strengths of 0.5 per cent accuracy

Mar 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.186..673b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 186, Mar. 1979, p. 673-684.

Other

63

Iron, Line Spectra, Solar Atmosphere, Solar Spectra, Abundance, Atmospheric Models, Atmospheric Turbulence, Oscillators

Scientific paper

The solar spectrum is interpreted using Oxford oscillator strengths for Fe I lines of excitation potential 0.00-1.01 eV of 0.5 percent accuracy. The analysis is used to test the accuracy of the oscillator strengths and to derive information about the solar atmosphere. Abundances and microturbulence values are deduced using the Vernazza, Arnett, and Loeser (1976) model atmosphere and three other model atmospheres. Using the Vernazza et al. model atmosphere at mu = 1.0, for the 0 eV lines the microturbulence is 0.78 km/s and the abundance log A = 7.440, and for 1 eV lines the values are 0.61 km/s and log A = 7.479, implying an increase in microturbulence with height. Microturbulence values for the integrated disk spectrum are 1.05 and 0.98 km/s, respectively. Until an acceptable model atmosphere is available the solar abundance of iron derived from the Fe I spectrum will remain uncertain by at least 0.2 dex. Damping coefficients are given for seven strong lines, and a curve of growth for the solar spectrum at mu = 1.0 is also given.

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