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The determination of lithium abundances in stars of young clusters have shownthat they deplete Li by different degrees during their pre-main sequence phase.Beryllium abundances are complementary to the lithium ones, and can helptracing the mixing processes in the stellar interiors. Our aim is to deriveberyllium abundances in a sample of G- and K-type stars of two young pre-mainsequence open clusters, IC 2391 and IC 2602. The Be abundances are used toinvestigate the mixing of internal material in these stars. The reliability ofthe Be lines as abundance indicators in low-temperatures is also investigatedin detail. We derived Be abundances from high-resolution, high signal-to-noiseUVES/VLT spectra using spectrum synthesis and model atmospheres. Atmosphericparameters and other elemental abundances are adopted from a previous work. Thesample stars have masses in the range between 0.80 < M/Msun < 1.20. They havebeen shown to differ in lithium abundance by about 0.60 dex, with lower A(Li)in cooler and lower mass stars. Here, we find that all the stars have the sameBe abundance within the uncertainties. These observations show that the Beabundance is not affected by the mixing events in the pre-main sequence, inthis mass range, in agreement with the expectation of evolutionary models. Acomparison with Be abundances in older clusters shows that, contrary to themodels, cool stars deplete Be during their main-sequence lifetime, confirmingwhat has been previously suggested in the literature.

Mixing at young ages: Beryllium abundances in cool main-sequence stars of the open clusters IC 2391 and IC 2602