On the solar abundance of indium

Abstract

The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical synthesis of the 451.13 nm line on which all indium abundance studies are based, both for the quiet-sun and the sunspot umbra spectrum, employing standard atmosphere models and accounting for hyperfine structure and Zeeman splitting in detail. The results, as well as a re-appraisal of indium nucleosynthesis, suggest that the solar indium abundance is close to the meteoritic value, and that some unidentified ion line causes the 451.13 nm feature in the quiet-sun spectrum.

arXiv comment7 pages, 9 figures, accepted for publication in MNRAS Main Journal

References in corpus (6)

• Neutron capture in low mass Asymptotic Giant Branch stars: cross sections and abundance signatures
• Galactic Evolution of Sr, Y, Zr: A Multiplicity of Nucleosynthetic Processes
• The Rise of the s-Process in the Galaxy
• Explorations of the r-Processes: Comparisons between Calculations and Observations of Low-Metallicity Stars
• On the Abundance of Holmium in the Sun
• The Sun's Interior Metallicity Constrained by Neutrinos

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