  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 \AA. 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.
