  The study of Be in stars of differing metal content can elucidate the
formation mechanisms and the Galactic chemical evolution of Be. We have
obtained high-resolution, high signal-to-noise spectra of the resonance lines
of Be II in eight stars with the high-dispersion spectrograph (HDS) on the
Subaru 8.2 m telescope on Mauna Kea. Abundances of Be have been determined
through spectrum synthesis. The stars with [Fe/H] values > -1.1 conform to the
published general trend of Be vs Fe. We have confirmed the high Be abundance in
HD 94028 and have found a similarly high Be abundance in another star, HD
132475, at the same metallicity: [Fe/H] = -1.5. These two stars are 0.5 - 0.6
dex higher in Be than the Be-Fe trend. While that general trend contains the
evidence for a Galaxy-wide enrichment in Be and Fe, the higher Be abundances in
those two stars indicates local Be enrichments. Possible enrichment mechanisms
include hypernovae and multiple supernova explosions contained in a
superbubble. The star G 64-37 has [Fe/] = -3.2; we have determined its Be
abundance to look for evidence of a Be plateau. It's Be abundance appears to
extend the Be-Fe trend to lower Fe abundances without any evidence for a
plateau as had been indicated by a high Be abundance in another very metal-poor
star, G 64-12. Although these two stars have similar Be abundances within the
errors, it could be that their different Be values may be indicating that a Be
dispersion exists even at the lowest metallicities.
