Carbon abundances in halo dwarfs

Details Carbon abundances in halo dwarfs Carbon abundances in halo dwarfs

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302..415t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 1, 1986, p. 415-420. Research supported by the Robert A. Welch F

Astronomy and Astrophysics

Astrophysics

57

Carbon Stars, Dwarf Stars, Metallicity, Stellar Composition, Stellar Spectra, Binary Stars, F Stars, G Stars, Milky Way Galaxy, Supernovae

Scientific paper

A spectrum synthesis analysis has been made of Digicon observations of CH in 32 halo F and G dwarfs with iron abundances as low as (Fe/H) approximately equal to -2.5. The results, combined with earlier results, also based on spectrum synthesis of Digicon CH spectra, show that carbon follows iron down to (Fe/H) about -1.8; at lower metallicities there is evidence of a positive trend in (C/Fe). It is suggested that the change in slope of the (C/Fe) vs (Fe/H) relationship at (Fe/H) about -1.8 is due to the appearance of Type I supernovae. The sense of the change of slope is consistent with the prediction that Type I supernovae are inefficient producers of carbon. More carbon abundances, determined from analysis of CH in even more metal-deficient stars and, also, determined from C I lines, are needed in order to establish the relationship between carbon and iron abundances in extremely metal-deficient (Fe/H less than about -2.0) dwarfs more firmly. One of the program stars (BD -0 degrees 4470) is found to be a double-lined spectroscopic binary composed of two nearly identical halo dwarfs.

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