Abundances in the Metal-poor Common Proper Motion Star BD +00 deg2058A

Details Abundances in the Metal-poor Common Proper Motion Star BD +00 deg2058A Abundances in the Metal-poor Common Proper Motion Star BD +00 deg2058A

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999pasp..111..817k&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 111, Issue 761, pp. 817-828.

Astronomy and Astrophysics

Astronomy

3

Stars: Binaries: General, Galaxy: Abundances, Galaxy: Halo, Stars: Abundances, Stars: Individual (Bd +00 Deg2058A), Stars: Late-Type, Stars: Population Ii

Scientific paper

Like two other metal-poor, late-type field stars showing odd abundance ratios suggestive of accreted origin, BD +00 deg2058A has a substantial apogalactocentric distance, reaches a large maximum height above the Galactic plane, and is a member of a common proper motion system. To examine whether such wide pairs might have a common origin in accreted subsystems, we present detailed abundances in BD +00 deg2058A derived from high signal-to-noise, high-resolution optical spectroscopy. Using spectroscopically derived parameters, we find [Fe/H]=-1.16+/-0.07, a factor of 2-4 larger than previous (but less direct) estimates. We find the alpha-element, iron-peak, and n-capture abundances to be unremarkable compared with other field stars of similar [Fe/H]. The derived Li abundance, logN(Li)=2.53, is large compared with otherwise similar stars; the normal n-capture abundances and upper limits to ^6Li/^7Li provide no evidence of Li enrichment from Li-rich asymptotic giant branch star material or spallation. Interestingly, the [C/Fe] and [Na/Fe] ratios appear to be ~0.3 dex lower and higher, respectively, than otherwise similar stars. This might point to Li enrichment by contaminating material having undergone ``cool bottom processing,'' but the lack of radial velocity variations provides no evidence of a close companion. Comparison with theoretical isochrones suggests a distance of 150 pc, which is in better agreement with two previous studies' estimates of the distance of the fainter wide companion; kinematically based population classifications based on this distance are ambiguous. Finally, we draw attention to the importance of different, but reasonable, choices of Fe I gf-values in our (and other) analyses.

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