Lithium synthesis in low metallicity AGB stars

Details Lithium synthesis in low metallicity AGB stars Lithium synthesis in low metallicity AGB stars

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1016..127i&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: The 10th International Symposium on Origin of Matter and Evolution of Galaxies: From

Other

Normal Galaxies, Extragalactic Objects And Systems, Giant And Subgiant Stars, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

We evolve thermally pulsing AGB star models in the mass range of 1-8 Msolar. The metallicity of the models is assumed to be [Fe/H]~=-3. Mass loss is taken into account to investigate the abundance patterns of the yields ejected from the AGB models. In the 1 and 2 Msolar AGB models hot bottom burning (HBB) does not take place at the base of the convective envelope during interpulse phases, but the low-mass models produce 7Li in an H-flash event. The occurrence of this event is associated with the ingestion of protons from the overlying H-rich envelope into the He-flash driven convective shell during thermal pulse phase. The resulting 7Li abundances are higher than the primordial one based on the analysis of the WMAP data. The present investigation also confirms the efficient production of 7Li by the HBB in the intermediate-mass (4-8 Msolar) AGB stars. If these AGB stars belong to a binary system with a low-mass companion, mass loss from the primary AGB star transfers the materials enriched in 7Li to the surface of the secondary star and makes the surface composition Li-rich. The formation of the Li-rich stars, however, strongly depends on the mass loss history and binary separation. The nucleosynthesis of the other light elements up to the phosphorus is also followed until the end of the AGB phase. We find that the yields of the low metallicity AGB stars well reproduce the abundance patterns of extremely metal-poor stars.

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