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2018MNRAS.477..421K - Mon. Not. R. Astron. Soc., 477, 421-437 (2018/June-2)

Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity.


Abstract (from CDS):

We present new theoretical stellar yields and surface abundances for asymptotic giant branch (AGB) models with a metallicity appropriate for stars in the Small Magellanic Cloud (SMC, Z = 0.0028, [Fe/H] ≃ -0.7). New evolutionary sequences and post-processing nucleosynthesis results are presented for initial masses between 1 and 7 M, where the 7 M is a super-AGB star with an O-Ne core. Models above 1.15 M become carbon rich during the AGB, and hot bottom burning begins in models M >= 3.75 M. We present stellar surface abundances as a function of thermal pulse number for elements between C to Bi and for a selection of isotopic ratios for elements up to Fe and Ni (e.g. 12C/13C), which can be compared to observations. The integrated stellar yields are presented for each model in the grid for hydrogen, helium, and all stable elements from C to Bi. We present evolutionary sequences of intermediate-mass models between 4 and 7 M and nucleosynthesis results for three masses (M = 3.75, 5, and 7 M) including s-process elements for two widely used AGB mass-loss prescriptions. We discuss our new models in the context of evolved AGB and post-AGB stars in the SMCs, barium stars in our Galaxy, the composition of Galactic globular clusters including Mg isotopes with a similar metallicity to our models, and to pre-solar grains which may have an origin in metal-poor AGB stars.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): nuclear reactions, nucleosynthesis, abundances - stars: AGB and post-AGB - ISM: abundances - galaxies: abundances - Magellanic Clouds

Simbad objects: 7

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