We present an analysis of both weak and strong lines of Mn I with well-defined profiles in the solar photosphere, using the accurate oscillator strengths measured at Oxford. In an LTE analysis with the Holweger and Müller model solar atmosphere a manganese abundance of log A = 5.39 at a microturbulence value of 0.85 km s−1 is found for the disc centre. Comparison of this result with the Oxford determination for the solar iron abundance shows an interesting discrepancy with the Fe/Mn ratio found in type C I meteorites.
No takes yet. Share an insight, caveat, or question.
Booth et al. (1984) studied this question.