The study of Be in stars of differing metal content can elucidate the formation mechanisms and the Galactic chemical evolution of the light element , 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-than-predicted Be abundances in those two stars shows that there are also local Be enrichments .
Possible enrichment mechanisms include hypernovae and multiple supernova explosions contained in a superbubble .
One of our stars , G 64-37 , has a very low metallicity of [ 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 are indicators of may be indicating that a Be dispersion even at the lowest metallicities .