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Abundance trends in heavier elements with evolutionary phase have been shownto exist in the globular cluster NGC 6752 [Fe/H]=-1.6. These trends are aresult of atomic diffusion and additional (non-convective) mixing. Studyingsuch trends can provide us with important constraints on the extent to whichdiffusion modifies the internal structure and surface abundances of solar-type,metal-poor stars. Taking advantage of a larger data sample, we investigate thereality and the size of these abundance trends and address questions andpotential biases associated with the various stellar populations that make upNGC6752. Based on uvby Str\"omgren photometry, we are able to separate threestellar populations in NGC 6752 along the evolutionary sequence from the baseof the red giant branch down to the turnoff point. We find weak systematicabundance trends with evolutionary phase for Ca, Ti, and Fe which are bestexplained by stellar-structure models including atomic diffusion with efficientadditional mixing. We derive a new value for the initial lithium abundance ofNGC 6752 after correcting for the effect of atomic diffusion and additionalmixing which falls slightly below the predicted standard BBN value. We findthree stellar populations by combining photometric and spectroscopic data of194 stars in the globular cluster NGC 6752. Abundance trends for groups ofelements, differently affected by atomic diffusion and additional mixing, areidentified. Although the statistical significance of the individual trends isweak, they all support the notion that atomic diffusion is operational alongthe evolutionary sequence of NGC 6752.

Atomic Diffusion and Mixing in Old Stars V: A deeper look into the Globular Cluster NGC 6752