A detailed abundance analysis is performed for four stars in M92 and two stars in M15 by using LTE line-blanketed model atmospheres. The deduced result of Fe/H with respect to the sun is -2.35 for M92 and -2.20 for M15. There are no obvious changes in the pattern of abundance as a function of atomic number except for a general lowering by a constant factor when M92 and M13 are compared. The dispersion in the Fe abundance of the M92 stars is very small. Implications for the mass and number of previous generations of stars and for mixing in the protoglobular cluster are discussed.
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Judith G. Cohen (1979) studied this question.