Other
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.5808k&link_type=abstract
American Astronomical Society, 188th AAS Meeting, #58.08; Bulletin of the American Astronomical Society, Vol. 28, p.916
Other
1
Scientific paper
We present high resolution high S/N spectra, obtained at the CTIO 4-m, of the Be II 3131 { Angstroms} region in the metal-rich solar analog α Cen A and its companion α Cen B. Be abundances are derived relative to the Sun in a consistent fashion via spectrum synthesis. For α Cen A, we find [Be/H]=+0.20{+/-}0.15 where the error reflects random uncertainties at the 1σ confidence level; systematic errors of { ~ }0.1 dex are also possible. Analysis of α Cen B is more uncertain since inadequacies in the linelist, which was calibrated with Solar data, may manifest themselves in cool metal-rich dwarfs. Our analysis suggests [Be/H]{la }+0.05. We also consider numerous uncertainties in the Solar photospheric and meteoritic Be abundances and conclude that it is likely the former value is depleted relative to the latter by 0.1-0.5 dex. Even a slight real depletion in solar photospheric Be coupled with the observed Li depletion of only { ~ }2 dex would favor a slow (possibly rotationally-induced) mixing mechanism in addition to standard model burning at the base of the convection zone. If the difference in the Be abundances of α Cen A and B is real, it too would strongly suggest the action of additional mixing mechanisms. The light element abundances of the Sun and α Cen A (and other Solar analogs) are not grossly dissimilar. Thus, the idea that standard models and the current solar photospheric Li and Be abundance are discrepant because the Sun is a lone ``oddball'' is doubtful. We consider the issue of the unidentified blending feature(s) in the 3131.065 { Angstroms} Be II region: a single significant blending feature could possibly fit the solar spectrum if it lies near λ3131.02.
Boesgaard Ann Merchant
Deliyannis Constantine P.
King Jeremy R.
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