Other
Scientific paper
Jan 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.293...89a&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 293, p. 89
Other
42
Heavy Elements, Abundance, S Stars, B Stars, K Stars, M Stars, Carbon Stars, Stellar Composition, Nuclear Fusion, Asymptotic Giant Branch Stars, Nonequilibrium Thermodynamics, Spectral Line Width, Rubidium
Scientific paper
We employ spectra of resolution 20-35,000 of seven SC stars, four S stars, two Ba stars, and two K-M stars to derive abundances of a variety of elements from Sr to Eu relative to iron. Special attention is paid to Rb and Tc, and to the ratio of the heavy s-process species to the light s-process elements. Abundances are derived in LTE, both by using model atmospheres in which the carbon and oxygen abundances are nearly equal and by using curves of growth. Spectrum synthesis is used for critical lines, such as the 5924-A line of Tc and the 7800-A line of Rb. For most of the heavy-element stars, the enhancement of the s-process elements is about a factor of 10. The ratio of the heavy to light s-process species is not far from solar, except for RR Her, for which the same ratio is + 0.45 dex. For Tc the blending by other lines is severe. While we have probably detected the 5924-A line, we can only present abundances in the less-than-or-equal-to category.
Abia Carlos
Wallerstein George
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