s-Process in Low Metallicity Stars: CEMP-s and CEMP-s+r

Details s-Process in Low Metallicity Stars: CEMP-s and CEMP-s+r s-Process in Low Metallicity Stars: CEMP-s and CEMP-s+r

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1001..131b&link_type=abstract

IXTH TORINO WORKSHOP ON EVOLUTION AND NUCLEOSYNTHESIS IN AGB STARS AND THE IIND PERUGIA WORKSHOP ON NUCLEAR ASTROPHYSICS. AIP C

Astronomy and Astrophysics

Astrophysics

4

Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Giant And Subgiant Stars, Abundances, Chemical Composition, Chemical Composition And Chemical Evolution, Population Ii Stars, Carbon Stars, S Stars, And Related Types

Scientific paper

A sample of 74 very metal-poor, C- and s-rich rich stars were collected from the literature. We give here a summary of the results obtained by comparing spectroscopic abundances of CEMP-s stars and AGB theoretical models, using different 13C-pocket efficiencies, initial masses and initial r-enrichments. They acquired the C and s enrichments by mass transfer in a close binary system from the more massive companion while on the AGB (now a white dwarf). In general, reasonable solutions are obtained for all the stars. About half of these objects have a relevant number of elements detected at high resolution spectroscopy, while only 10 of them were obtained at moderate resolution. When few elements were detected, several solutions are possible. For most of the main-sequence turnoff stars, due to the low Na and, in some cases, the low ls peak (Sr-Y-Zr), a good interpretation can only be obtained with lower initial AGB masses (MiniAGB<=1.4 Msolar), and the absence of dilution factors suggests that no efficient thermohaline mixing had occurred. Among the stars with r-elements measured, an important number is r-enhanced (~46%), including six objects which need a strong initial r-enrichment ([r/Fe]ini = 2.0 dex). We show here some examples.

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