Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..226s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 226-232. Research supported by the Robert A. Welch F
Astronomy and Astrophysics
Astrophysics
23
Abundance, Binary Stars, Giant Stars, Late Stars, Lithium, Stellar Evolution, Subgiant Stars, Asymptotic Giant Branch Stars, Main Sequence Stars, Mass Transfer, Stellar Composition, Stellar Envelopes, Stellar Luminosity, Stellar Spectrophotometry
Scientific paper
Lithium abundances in 10 subgiant CH stars and one giant CH star are reported. In no star was the Li I resonance doublet detected, and upper limits to the lithium abundance in the range log epsilon-(Li) of no more than 0.7 to log epsilon(Li) = 1.5 /log epsilon(H) = 12.0/ were determined for this sample of stars. The subgiant CH stars are on, or near, the main sequence, and as they evolve up the red giant branch, the deepening convective envelopes will dilute lithium by a factor of about 30-50. This dilution factor, along with the upper limits to the current lithium abundances, would give the subgiant CH stars when they become red giants distinctly lower Li abundances than are observed in the classical barium stars. This suggests that subgiant CH stars are not progenitors of the classical barium stars. As the subgiant CH stars do show C-12 and s-process enhancements and are all binaries with low-luminosity companions, they may represent mass transfer from a former asymptotic giant branch star (now a white dwarf) onto a main-sequence companion (now a subgiant CH star).
Lambert David L.
Smith Verne V.
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