The abundance of nine elements is determined relative to hydrogen, using the observations of the forbidden lines in the corona obtained principally at the eclipse of 1952 February 25. The errors inherent in the analysis, those of observation, physical parameters, and theoretical assumption, are discussed in detail. An empirical method is developed for finding the total abundance of an element when only a single stage of ionization is observed. The results indicate disagreement with the photospheric abundances but good agreement with the meteorite compositions.