Abstract
It is well established that stellar element abundances show a variation of some ratios, such as oxygen to iron and calcium to iron, with the overall metallicity of the star. This has been ascribed to a time-delay effect due to the different mean lifetimes of the stars and binaries that give rise to Type II and Type I supernovae. It is proposed that this identification may be premature, and that the observations could equally well be explained by a pseudo-secondary behaviour in the nucleosynthesis of iron
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