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1982•Monthly Notices of the Royal Astronomical SocietyOpen access

Note on the interpretation of Fe I lines (2.18-2.49 eV) in the solar spectrum

D. E. Blackwell, M. J. Shallis, Gustavus J. Simmons

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Abstract

Fourteen Fe I lines |$(2.18\,\text{eV}\,\lt\,\chi \,\lt2.4\,\text{eV})$| in the centre of disc solar spectrum are analysed using Oxford oscillator strengths of 1 per cent accuracy. The iron abundances and micro turbulence velocities given by these lines are discussed. The five lines with excitation energies 2.40–2.48 eV apparently give a higher abundance than the nine lines of excitation energy 2.18–2.22 eV.

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Fourteen Fe I lines |$(2.18\,\text{eV}\,\lt\,\chi \,\lt2.4\,\text{eV})$| in the centre of disc solar spectrum are analysed using Oxford oscillator strengths of 1 per cent accuracy. The iron abundances and micro turbulence velocities given by these lines are discussed. The five lines with excitation energies 2.40–2.48 eV apparently give a higher abundance than the nine lines of excitation energy 2.18–2.22 eV.

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Available abstract

Fourteen Fe I lines |$(2.18\,\text{eV}\,\lt\,\chi \,\lt2.4\,\text{eV})$| in the centre of disc solar spectrum are analysed using Oxford oscillator strengths of 1 per cent accuracy. The iron abundances and micro turbulence velocities given by these lines are discussed. The five lines with excitation energies 2.40–2.48 eV apparently give a higher abundance than the nine lines of excitation energy 2.18–2.22 eV.

Key concepts: Physics, Excitation, Spectral line, Atomic physics, Astrophysics, Interpretation (philosophy), Solar atmosphere, Spectrum (functional analysis)

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