  The process of convective settling is based on the assumption that a small
fraction of the low-entropy downflows sink from the photosphere down to the
bottom of the star's envelope convection zone retaining a substantial entropy
contrast. We have previously shown that this process could explain the slow Li
depletion observed in the Sun. We construct a parametric model of convective
settling to investigate the dependence of Li and Be depletion on stellar mass
and age. Our model is generally in good agreement with the Li abundances
measured in open clusters and solar twins, although it seems to underestimate
the Li depletion in the first ~1 Gyr. The model is also compatible with the Be
abundances measured in a sample of field stars.
