Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity. Issue 1 (14th March 2018)

• Record Type: Journal Article
• Authors: Karakas, Amanda I; Lugaro, Maria; Carlos, Marília; Cseh, Borbála; Kamath, Devika; García-Hernández, D A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 477:Issue 1(2018)
• Page Start: 421
• Page End: 437
• Publication Date: 2018-03-14
• Subjects: nuclear reactions, nucleosynthesis, abundances -- stars: AGB and post-AGB -- ISM: abundances -- galaxies: abundances -- Magellanic Clouds; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty625
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: 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. 12 C/ 13 C), 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.