Evolution of the S-element abundances of 3-solar-mass asymptotic giant branch stars

Details Evolution of the S-element abundances of 3-solar-mass asymptotic giant branch stars Evolution of the S-element abundances of 3-solar-mass asymptotic giant branch stars

Sep 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997acasn..38..231z&link_type=abstract

Acta Astronomica Sinica, vol. 38, p. 231

Astronomy and Astrophysics

Astronomy

3

Asymptotic Giant Branch Stars, Nuclear Fusion, S Stars, Shell Stars, Stellar Composition, Helium, Stellar Evolution

Scientific paper

A comparison is presented between the predictions of nucleosynthesis calculations for Population I low-mass stars during the He-shell flashes of the asymptotic giant branch (AGB) and the distribution of heavy elements and C/O ratios observed in MS, S, and C stars. By varying the main parameters within the range allowed by present models a large set of results is constructed, covering the range in neutron exposures from tau(0) = 0.2 to tau(0) = 0.6/mb. The M to S to C evolutionary sequence is supported by the comparison between the predictions by calculation and the observations. The photospheric abundances of AGB stars are shown to be dependent not only on the neutron exposure achieved in the He shell, but also on how and when the third dredge-up actually occurs. The influence of main parameters on predictions is also discussed.

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