  Boron provides a special probe below the stellar surface as it survives to
greater depths than do Li and Be. To search for B depletions we have observed B
in 13 F and G dwarfs with large Be depletions; for comparison we also obtained
spectra of five stars which are undepleted in Li and Be. We have used HST with
STIS to obtain spectra of the B I resonance line at 2497 \AA. The spectral
resolution is 30,000 or 114,000 and the median signal-to-noise ratio is 70 per
pixel. New Be and Li spectra have been obtained at Keck I with HIRES of four of
the five standard stars at $\sim$48,000 resolution. Abundances have been
determined by the spectrum synthesis method with MOOG. A comparison between the
standard stars and those with severe Be depletions shows a distinct difference
in the B abundances between the two groups of 0.22 dex. We have discovered a
correlation between the Be and B abundances. The slope between A(Be) and
A(B)$_{NLTE}$ is 0.22 $\pm$0.05 (where A(element) = log N(element)/N(H) +
12.00) which, as expected, is shallower than the slope between A(Li) and A(Be)
of 0.38. We have normalized the light element abundances to account for the
observation that the initial abundances are somewhat lower in lower metallicity
stars by employing recently published empirical relations between Be and [Fe/H]
and between B and [Fe/H] (Boesgaard et al). The correlation between the
normalized A(Be) and A(B)$_{NLTE}$ has a slope of 0.18 $\pm$0.06. The star with
the largest Be depletion, HR 107 a main sequence Ba star, also has the largest
B depletion with the B abundance lower by a factor of 3.5 relative to the
standard stars.
