Beryllium in Disk and Halo Stars -- Evidence for a Beryllium Dispersion in Old Stars

Details Beryllium in Disk and Halo Stars -- Evidence for a Beryllium Dispersion in Old Stars Beryllium in Disk and Halo Stars -- Evidence for a Beryllium Dispersion in Old Stars

2005-12-13

arxiv.org/abs/astro-ph/0512317v1

Astrophys.J.641:1122-1130,2006

Astronomy and Astrophysics

Astrophysics

Accepted for Ap.J. 25 pages, including 7 figures and 3 tables

Scientific paper

10.1086/500501

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.

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