Spectrograms of the Be II resonance lines at 3130.4 and 3131.1 A in several Hyades dwarfs and four Hyades yellow giants are used to determine whether the constancy in Be abundance found for field stars extends to cluster stars, to test whether Be content is a function of stellar age, and to measure the amount of post-main-sequence dilution that has occurred in the yellow giants. A model-atmosphere abundance program is employed to obtain the Be/H ratio, which is found to be no more than 3.1 by 10 to the -13th power for the giants and approximately 10 to the -11th power for the dwarfs. On the average, the giants are shown to be deficient in Be relative to the dwarfs by a factor of at least 30. Analysis of light-element dilution in the giants provides indirect evidence that mass loss probably takes place before the convective envelope has expanded significantly. It is concluded that the Hyades dwarfs have the same Be content as the field stars, the Be abundance exhibits little variation with time, and evidence for astration is extremely marginal at best.