The AL I-cyanogen correlation in the spectra of globular cluster red giants and the origin of intracluster heavy element variations

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Cyanogen, Globular Clusters, Late Stars, Red Giant Stars, Stellar Spectra, Abundance, Aluminum, Heavy Elements, Horizontal Branch Stars, Line Spectra, Metallicity, Nuclear Fusion

Scientific paper

A possible positive correlation between the behavior of the Al I resonance lines at 3944 and 3965 A and the behavior of the CN bands, as reported for the case of NGC 6752, is investigated by means of a spectroscopic survey of CN-strong/CN-weak pairs of star groupings in seven globular clusters. The correlation is found to exist in five of the clusters, while in the cases of M4 and 47 Tucanae the Al I lines appear not to vary between the CN-strong and CN-weak groups. The implications of these results and other abundance patterns of these systems for the origin of intracluster C, N, Na, Al, and heavy s-process element variations are considered. It is conjectured that the difference in the behavior of C and the heavy s-process elements between Omega Centauri and M22, on one hand, and such clusters as NGC 6752 on the other, is that enrichment in the former was provided by the ejecta from stars whose mass function extended to lower mass than in the latter.

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