Differences in C/O distributions of carbon stars as an indicator of the inhomogeneity of chemical composition in the Galaxy

Details Differences in C/O distributions of carbon stars as an indicator of the inhomogeneity of chemical composition in the Galaxy Differences in C/O distributions of carbon stars as an indicator of the inhomogeneity of chemical composition in the Galaxy

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998arep...42..193f&link_type=abstract

Astronomy Reports, Volume 42, Issue 2, March 1998, pp.193-199

Astronomy and Astrophysics

Astronomy

Scientific paper

The C/O ratio in the atmospheres of N carbon stars in the Perseus and Orion arms of the Galaxy have been obtained using moderate-dispersion spectrograms. The resulting C/O distributions for these arms are different. Theoretical C/O distributions are determined using synthetic population calculations for asymptotic giant branch carbon stars. The following three ways in which heavy-element abundances influence C/O distributions are considered: the rate of increase of C/O during each burning flare of the helium shell source, the mass-loss rate, and the minimum mass of a star at which the `third dredge-up' is possible. All three factors influence the results in the same way: the number of carbon stars with high C/O ratios and the dispersion of the C/O ratio about the value C/O = 1 both decrease with increase in the heavy-element abundance. Comparison of the calculations with the observational results indicates that the Perseus arm has a higher heavy-element abundance than the Orion arm.

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