Progresses in AGB Modelling

Details Progresses in AGB Modelling Progresses in AGB Modelling

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1001....3c&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

2

Origin, Formation, And Abundances Of The Elements, Giant And Subgiant Stars, Carbon Stars, S Stars, And Related Types, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Abundances, Chemical Composition

Scientific paper

The full understanding of final stellar evolution phases is a fundamental request to properly investigate the Universe at any temporal and spatial scale. While the theoretical scenarios of H- and He-burning have been deeply investigated in the last 30 years, the modelling of stellar evolution beyond the core-helium burning phase and the related nucleosynthesis still present problems related to the physics and to the numerical methods. Low mass AGB Stars (1Among the most important results we achieved, we highlight the explanation of the mechanism of neutron production, which controls the s-process nucleosynthesis in low-mass AGB, the coupling of the code with a full nuclear network, from H up to Pb-Bi (at the termination point of the s-process path) and the introduction of C-enhanced low temperature opacities, whose effects are particularly important at low metallicities. In this paper, we describe the current state of the art of our modelling and we present detailed models of low mass AGB (M = 2Msolar) stars at different metallicities (from Z = Zsolar to Z = 10-4). The final elemental distributions we find are representative of the ones expected for the intrinsic carbon stars observed in the disk and in the halo of the Milky Way.

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