A DETERMINATION OF THE SOLAR ABUNDANCE OF IRON FROM THE STRONG LINES OF FE-I

The solar abundance of iron is determined from strong lines of Fe I wi th well-determined f-values using collision-damping constants for the lines from the theory of Anstee & O'Mara. The derived abundance is ind ependent of non-thermal motions in the solar photosphere and is in exc ellent agreement with the meteoritic abundance of iron. ?he results ar e discussed in the light of recent determinations of the abundance bas ed on medium-strong lines of Fe I which have been a subject of some co ntroversy. The results are also used to assess the accuracy of the lin e-broadening theory.