Abstract

Spectrograms of 6.7 A mm/sup -1/ have been obtained of six dwarfs and four giants in the Hyades Cluster to determine the Be/H content from one of the Be II resonance lines, lambda3131.064. A model-atmosphere abundance program was used which yielded a mean Be/H of 1.0 x 10/sup -11/ for the dwarfs and < or =3.1 x 10/sup -13/ for the giants. The Be content of the cluster dwarfs agrees well with that of field stars found by Boesgaard. The Be in both field stars and the Hyades can be explained through galactic--cosmic-ray (GCR) spallation reactions. The Li/Be ratio in the Hyades dwarfs is 80, in agreement with the cosmic Li/Be. Both Be and Li are deficient in the giants compared with their abundances in the dwarfs. A combination of post--main-sequence mass loss and dilution from any expanding convective envelope is required to explain the observed deficiencies. A mass-loss rate of 8 x 10/sup -11/ M/sub sun/ yr/sup -1/ appears to be sufficient.

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