Abstract
The chemical evolution history of clusters is a complex scenario. The interplay between star formation, stellar evolution (with mass loss), and cluster dynamical evolution must be considered. Critical tests would be to derive abundances in dwarfs and lower RGB stars, and compare them with those obtained for upper RGB stars; this may clear the role of mixing, and give precious information about dilution at the base of the R,GB, that is important to understand if pollution and diffusion are indeed important. This is now possible thanks to UVES at VLT.
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Gratton, R.G. (2000). Metal Abundances in Globular Clusters. In: Matteucci, F., Giovannelli, F. (eds) The Evolution of The Milky Way. Astrophysics and Space Science Library, vol 255. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0938-6_16
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DOI: https://doi.org/10.1007/978-94-010-0938-6_16
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