Abstract
The solar abundance of iron is determined from strong lines of Fe I with well-determined f-values using collision-damping constants for the lines from the theory of Anstee & O'Mara. The derived abundance is independent of non-thermal motions in the solar photosphere and is in excellent agreement with the meteoritic abundance of iron. The results are discussed in the light of recent determinations of the abundance based on medium-strong lines of Fe I which have been a subject of some controversy. The results are also used to assess the accuracy of the line-broadening theory.
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