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A. M. Boesgaard (U. Hawaii)
The abundance of Li is known for a large number of F and G dwarfs in the field and in open clusters. The Li information from clusters of different ages and metallicities is particularly useful in ascertaining the mechanisms that may lead to the surface depletion of Li. The standard, non-rotating, evolutionary models of F and G dwarfs are not sufficient to explain the observed abundances. In contrast with Li there is relatively little information on the Be abundances, especially in G stars, both in clusters and in the field. But information on the abundances of the two elements together provide far more powerful indicators for the building of model stars and for learning about the probable causes of light element depletion. Here we report on new Keck/HIRES observations of Be. We have determined Be abundances for 25 Hyades dwarfs with known Li abundances distributed over a temperature range of 5400 - 6600 K. In addition we have observed Be in 7 Pleiades stars, 3 Praesepe stars and 36 field stars, all with known Li abundances.