Synthesis of lithium and s-process elements in Small Magellanic Cloud asymptotic giant branch stars

Details Synthesis of lithium and s-process elements in Small Magellanic Cloud asymptotic giant branch stars Synthesis of lithium and s-process elements in Small Magellanic Cloud asymptotic giant branch stars

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...345l..75s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 345, Oct. 15, 1989, p. L75-L78. Research supported by the Robert

Astronomy and Astrophysics

Astrophysics

140

Abundance, Asymptotic Giant Branch Stars, Late Stars, Magellanic Clouds, Nuclear Fusion, Red Giant Stars, Astronomical Spectroscopy, Lithium, Quantitative Analysis, Stellar Evolution, Zirconium Oxides

Scientific paper

High-resolution spectroscopy is presented for five luminous asymptotic giant branch (AGB) stars in the SMC. These stars are found to be metal-poor (Fe/H of about -0.5) but s-process-enriched, relative to Fe-peak elements, by up to a factor of 10: these are s-process enhancements that are comparable to those observed in Galactic S stars; thus, these SMC AGB stars have experienced a third dredge-up. Of more interest is the fact that all five red giants have rather strong Li I resonance lines (6707 A); an abundance analysis reveals these stars to have Li abundances that are 100-1000 times that expected in red giants. These very luminous (and probably massive) AGB stars are argued to have synthesized Li as predicted by certain stellar models of hot-bottom convective-envelope burning. The observations and models are discussed as a basis for understanding certain phases of red giant evolution and as a potentially significant source of Li in the universe.

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