Interpretation of CEMP(s) and CEMP(s + r) Stars with AGB Models

Details Interpretation of CEMP(s) and CEMP(s + r) Stars with AGB Models Interpretation of CEMP(s) and CEMP(s + r) Stars with AGB Models

2009-09-18

arxiv.org/abs/0909.3454v1

PASA 2009 Volume 26 Number 3, pp. 314-321

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

8 pages, 6 figures, 2 tables

Scientific paper

10.1071/AS08055

Asymptotic Giant Branch (AGB) stars play a fundamental role in the s-process nucleosynthesis during their thermal pulsing phase. The theoretical predictions obtained by AGB models at different masses, s-process efficiencies, dilution factors and initial r-enrichment, are compared with spectroscopic observations of Carbon-Enhanced Metal-Poor stars enriched in s-process elements, CEMP(s), collected from the literature. We discuss here five stars as example, CS 22880-074, CS 22942-019, CS 29526-110, HE 0202-2204, and LP 625-44. All these objects lie on the main-sequence or on the giant phase, clearly before the TP-AGB stage: the hypothesis of mass transfer from an AGB companion, would explain the observed s-process enhancement. CS 29526-110 and LP 625-44 are CEMP(s+r) objects, and are interpreted assuming that the molecular cloud, from which the binary system formed, was already enriched in r-process elements by SNII pollution. In several cases, the observed s-process distribution may be accounted for AGB models of different initial masses with proper 13C-pocket efficiency and dilution factor. Na (and Mg), produced via the neutron capture chain starting from 22Ne, may provide an indicator of the initial AGB mass.

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