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Determinations of beryllium abundance in stars, together with lithium,provide a key tool to investigate the so far poorly understood extra-mixingprocesses at work in stellar interiors. We measured Be in three openclusters,complementing existing Be surveys, and aiming at gathering a morecomplete empirical scenario of the evolution of Be as a function of stellar ageand temperature. Specifically, we analyzed VLT/UVES spectra of members of NGC2516, the Hyades, and M 67 to determine their Be and Li abundances. In thefirst two clusters we focused on stars cooler than 5400 K, while the M 67sample includes stars warmer than 6150 K, as well as two subgiants and two bluestragglers. We also computed the evolution of Be for a 0.9 Mo star based onstandard evolutionary models. We find different emprical behaviours for starsin different temperature bins and ages. Stars warmer than 6150 K show Bedepletion and follow a Be vs. Li correlation while Be is undepleted in stars inthe ~6150-5600 K range. NGC 2516 members cooler than 5400 K have not depletedany Be, but older Hyades of similar temperature do show some depletion. Be isseverely depleted in the subgiants and blue stragglers. The results for warmstars are in agreement with previous studies, supporting the hypothesis thatmixing in this temperature regime is driven by rotation. The same holds for thetwo subgiants that have evolved from the "Li gap". This mechanism is insteadnot the dominant one for solar-type stars. We show that Be depletion of coolHyades cannot simply be explained by the effect of increasing depth of theconvective zone. Finally, the different Be content of the two blue stragglerssuggests that they have formed by two different processes (i.e., collisions vs.binary merging).

Tracing mixing in stars: new beryllium observations of the open clusters NGC 2516, Hyades, and M67