Astronomy and Astrophysics – Astronomy
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aj....109.2204t&link_type=abstract
Astronomical Journal v.109, p.2204
Astronomy and Astrophysics
Astronomy
56
Stars: Abundances, Galaxy: Abundances, Stars: Carbon
Scientific paper
We have determined C abundances from observations of the 7100 Å C I lines in 105 field disk F and U main-sequence stars. We use the results to investigate the enrichment of C in the Galactic disk over the range -0.8≤[Fe/H]≤+0.2. A moderate enrichment of C in metal-deficient stars, such that [C/Fe]˜+0.20±0.05 at [Fe/H]=-0.8, is found. This is consistent with the results of earlier investigations based on more limited samples of stars. With the aid of ages and galactocentric distances for the same stars determined by Edvardsson et al. (1993), we examine the relation between stellar age and C abundance. For stars in the same range of galactocentric distance, we find only a weak correlation between the stars' C abundances and their ages. The moderate enrichment of C in metal-deficient disk stars is qualitatively similar to that seen for O and the a elements. We compare the behavior of the stellar [C/Fe], [0/Fe], and [a/Fe] abundances as functions of metallicity (using O and α element abundances from Edvardsson et al.), with the predictions of Timmes et al. `s [ApJS (in press) (1995)] new models of Galactic chemical evolution. The comparison confirms Timmes et al. `s conclusion that, with regard to the variation of these abundances with metallicity, the best agreement between observation and theory is provided by models in which the iron yields of II supernovae are reduced by a factor of 2 below the (uncertain) value adopted for their standard models. A similar comparison of the [C/O] and [C/α] abundances, which are much less sensitive to the Type II supernovae iron yields, as functions of metallicity, shows substantial agreement of observation and theory.
Lambert David L.
Lemke Michael
Tomkin Jocelyn
Woolf Vincent M.
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