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 ≥ 3.75M⊙. 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 7M⊙) including s-process elements for two widely used AGB mass-loss prescriptions.We discuss our newmodels in the context of evolvedAGB 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.
| Language | English |
|---|---|
| Pages | 421-437 |
| Number of pages | 17 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 477 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 11 Jun 2018 |
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Keywords
- nuclear reactions, nucleosynthesis, abundances
- stars: AGB and post-AGB
- ISM: abundances
- galaxies: abundances
- Magellanic Clouds
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Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity. / Karakas, Amanda I.; Lugaro, Maria; Carlos, Marília; Cseh, Borbála; Kamath, Devika; García-Hernández, D. A.
In: Monthly Notices of the Royal Astronomical Society, Vol. 477, No. 1, 11.06.2018, p. 421-437.Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - Heavy-element yields and abundances of asymptotic giant branch models with a Small Magellanic Cloud metallicity
AU - Karakas, Amanda I.
AU - Lugaro, Maria
AU - Carlos, Marília
AU - Cseh, Borbála
AU - Kamath, Devika
AU - García-Hernández, D. A.
PY - 2018/6/11
Y1 - 2018/6/11
N2 - 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 ≥ 3.75M⊙. 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 7M⊙) including s-process elements for two widely used AGB mass-loss prescriptions.We discuss our newmodels in the context of evolvedAGB 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.
AB - 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 ≥ 3.75M⊙. 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 7M⊙) including s-process elements for two widely used AGB mass-loss prescriptions.We discuss our newmodels in the context of evolvedAGB 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.
KW - nuclear reactions, nucleosynthesis, abundances
KW - stars: AGB and post-AGB
KW - ISM: abundances
KW - galaxies: abundances
KW - Magellanic Clouds
UR - http://www.scopus.com/inward/record.url?scp=85046650204&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty625
DO - 10.1093/mnras/sty625
M3 - Article
VL - 477
SP - 421
EP - 437
JO - Monthly Notices of the Royal Astronomical Society
T2 - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -