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AGB stars have long been held responsible for the important star-to-starvariations in light elements observed in Galactic globular clusters. We analysethe main impacts of a first generation of rotating intermediate-mass stars onthe chemical properties of second-generation globular cluster stars. Therotating models were computed without magnetic fields and without the effectsof internal gravity waves. They account for the transports by meridionalcurrents and turbulence. We computed the evolution of both standard androtating stellar models with initial masses between 2.5 and 8 Msun within themetallicity range covered by Galactic globular clusters. During centralHe-burning, rotational mixing transports fresh CO-rich material from the coretowards the hydrogen-burning shell, leading to the production of primary 14N.In stars more massive than M > 4 Msun, the convective envelope reaches thisreservoir during the second dredge-up episode, resulting in a large increase inthe total C+N+O content at the stellar surface and in the stellar wind. Thecorresponding pollution depends on the initial metallicity. At low- andintermediate-metallicity, it is at odds with the constancy of C+N+O observedamong globular cluster low-mass stars. With the given input physics, our modelssuggest that massive rotating AGB stars have not shaped the abundance patternsobserved in low- and intermediate-metallicity globular clusters. Ournon-rotating models, on the other hands, do not predict surface C+N+Oenhancements, hence are in a better position as sources of the chemicalanomalies in globular clusters showing the constancy of the C+N+O. However atthe moment, there is no reason to think that intermediate mass stars were notrotating.

CNO enrichment by rotating AGB stars in globular clusters