We have determined Be abundances in 50 F and G dwarfs in the mass range of 0.9 \leq M _ { \odot } \leq 1.1 as determined by Lambert & Reddy .
The effective temperatures are 5600 to 6400 K and metallicities from - 0.65 to +0.11 .
The spectra were taken primarily with Keck I + HIRES .
The Be abundances were found via spectral synthesis of Be II lines near 3130 Ã .
The Be abundances were investigated as a function of age , temperature , metallicity and Li abundance in this narrow mass range .
Even though our stars are similar in mass , they show a range in Be abundances of a factor of > 40 .
We find that [ Be/Fe ] has no dependence on temperature , but does show a spread of a factor of 6 at a given temperature .
The reality of the spread is shown by two identical stars which differ from each other by a factor of two only in their abundances of Li and Be .
Our thin-disk-star sample fits the trend between Be abundance and [ Fe/H ] found for halo and thick disk stars , extending it to about 4 orders of magnitude in the two logarithmic quantities .
Both Fe and Be appear to increase similarly over time in the Galaxy .
One-third of our sample may be classified as subgiants ; these more-evolved stars have lower Be abundances than the dwarfs .
They have undergone Be depletion by slow mixing on the main sequence and Be dilution during their trip toward the red giant base .
There are both Li and Be detections in 60 field stars in the “ Li-plateau ” of 5900 - 6300 K now and the abundances of the two light elements are correlated with a slope of 0.34 \pm 0.05 , with greater Li depletion than Be depletion .