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Abundance anomalies have been determined at the surface of many field andopen cluster A and F dwarfs. These abundance anomalies are most likely causedby microscopic diffusion at work within the stable envelopes of A stars.However diffusion can be counteracted by several other mixing processes such asconvection, rotational mixing and mass loss. We present a short review of thesurface abundance patterns of A/F stars in the Pleiades (100 Myr), ComaBerenices (450 Myr) and Hyades (650 Myr) open clusters. Real star-to-starvariations of the abundances were found for several chemical elements in the Adwarfs in these clusters. The derived abundances are then compared toevolutionary models from the Montreal group. These comparisons strongly suggestthe occurence of hydrodynamical processes at play within the radiative zones ofthese stars and hindering the effects of microscopic diffusion (mixingprocesses/mass loss). In the frame of Gaia mission, simulations are presentedthat predict the number of A stars and open clusters that Gaia will observe inthe Galaxy.

Chemically Peculiar A/F Stars in Open Clusters of the Milky Way