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We have determined Be abundances in 50 F and G dwarfs in the mass range of0.9 $\leq$ M$_\odot$ $\leq$ 1.1 as determined by Lambert & Reddy. The effectivetemperatures are 5600 to 6400 K and metallicities from $-$0.65 to +0.11. Thespectra were taken primarily with Keck I + HIRES. The Be abundances were foundvia spectral synthesis of Be II lines near 3130 \AA. The Be abundances wereinvestigated as a function of age, temperature, metallicity and Li abundance inthis narrow mass range. Even though our stars are similar in mass, they show arange in Be abundances of a factor of $>$40. We find that [Be/Fe] has nodependence on temperature, but does show a spread of a factor of 6 at a giventemperature. The reality of the spread is shown by two identical stars whichdiffer from each other by a factor of two only in their abundances of Li andBe. Our thin-disk-star sample fits the trend between Be abundance and [Fe/H]found for halo and thick disk stars, extending it to about 4 orders ofmagnitude in the two logarithmic quantities. Both Fe and Be appear to increasesimilarly over time in the Galaxy. One-third of our sample may be classified assubgiants; these more-evolved stars have lower Be abundances than the dwarfs.They have undergone Be depletion by slow mixing on the main sequence and Bedilution during their trip toward the red giant base. There are both Li and Bedetections in 60 field stars in the "Li-plateau" of 5900 - 6300 K now and theabundances of the two light elements are correlated with a slope of 0.34$\pm$0.05, with greater Li depletion than Be depletion.

Beryllium Abundances in Stars of One-Solar-Mass