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Low-Mass Extremely Metal-Poor Stellar Models: Yields, Uncertainties and the Galactic Halo Stars

Published online by Cambridge University Press:  01 April 2008

Simon W. Campbell  and
J. C. Lattanzio
Simon W. Campbell
Affiliation:
Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei, Taiwan10617 email: [email protected] Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Melbourne, Australia 3800 email: [email protected]
J. C. Lattanzio
Affiliation:
Academia Sinica Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei, Taiwan10617 email: [email protected]
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Abstract

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We have calculated a set of low-mass (0.85 M⊙ ≤ M ≤ 3.0 M⊙) zero metallicity and extremely metal-poor (−6.5 ≤ [Fe/H] ≤ −3.0) stellar models, including nucleosynthetic yields for 74 species. As far as we are aware these are the first detailed yields in the mass and metallicity range considered. Due to the difficulty in modelling such stars the yields naturally contain numerous uncertainties, and thus present interesting challenges for future stellar modelling. We briefly present some results in the context of the Galactic Halo star observations, and also discuss qualitatively some of the uncertainties in the modelling. We conclude by suggesting that much work is still necessary in this research area. For example, multidimensional fluid dynamics models are needed to simulate the violent proton ingestion events that occur during the core He flash and early TPAGB, observations and theory of mass loss at low metallicities are needed, the effects of reaction rate uncertainties need to be quantified, and low temperature opacities variable in carbon (and nitrogen) need to be included in the models.

Keywords

stars: AGB and post-AGBstars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 235 - 241
Copyright
Copyright © International Astronomical Union 2008

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