Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters
By P. Ventura, M. Criscienzo, R. Carini, F. D’Antona. 2013
193 citations recorded by the source corpus.
We present yields from stars of mass in the range Mo<M<8Mo of metallicities Z=0.0003 and Z=0.008, thus encompassing the chemistry of low- and high-Z Globular Clusters. The yields are based on full evolutionary computations, following the evolution of the stars from the pre-Main Sequence through the Asymptotic Giant Branch phase, until the external envelope is lost. Independently of metallicity, stars with M<3Mo are dominated by Third Dredge-Up, thus ejecting into their surroundings gas enriched in carbon and nitrogen. Conversely, Hot Bottom Burning is the main responsible for the modification of the surface chemistry of more massive stars, whose mass exceeds 3Mo: their gas shows traces of proton-capture nucleosynthesis. The extent of Hot Bottom Burning turns out to be strongly dependent on metallicity. In this paper we analyze the consequences of this fact. These results can be used to understand the role played by intermediate mass stars in the self-enrichment scenario of globular clusters: the results from spectroscopic investigations of stars belonging to the second generation of clusters with different metallicity will be used as an indirect test of the reliability of the present yields. The treatment of mass loss and convection are confirmed as the main uncertainties affecting the results obtained in the context of the modeling of the thermal pulses phase. An indirect proof of this comes from the comparison with other investigations in the literature, based on a different prescription for the efficiency of convection in transporting energy and using a different recipe to determine the mass loss rate.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/05731ab6cb121de74502fdfd43be04bf335fdc73
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Citations in the corpus
- GALACTIC CHEMICAL EVOLUTION AND SOLAR s-PROCESS ABUNDANCES: DEPENDENCE ON THE 13C-POCKET STRUCTURE (2014, background): “The mass and metallicity limits of SAGB depend on models, and the treatment of core carbon ignition and burning and the efficiency of the TDU are very uncertain (e.g., Siess 2010; Ventura et al. 2013).”
- The Hubble Space TelescopeUV Legacy Survey of Galactic Globular Clusters – V. Constraints on formation scenarios (2015, background): “Indeed, during their AGB phase stars in the mass range∼ 3 − 4 M⊙ to ∼ 8 M⊙ experience the so called hot bottom burning (HBB) process (see e.g., Ventura et al. 2013, whereby very high temperatures are reached at the bottom of the convective envelope, thus allowing efficient p-capture nuclear…”
- The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, background): “There is an extensive literature on the problem (Cottrell & Da Costa 1981; Pumo et al. 2008; Ventura & D’Antona 2009, 2010; D’Ercole et al. 2010, 2011; Ventura & D’Antona 2011; Ventura et al. 2011; D’Ercole et al. 2012; D’Antona et al. 2012; Ventura et al. 2012, 2013; Doherty et al. 2014b).”
- Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, methodology): “…that 9 These models assume an exponential decay of convective velocities starting from convective boundaries, with the e-folding distance given by ζHP with ζ =0.02 (Ventura et al. 2013). the EC-SN channel is limited to a very narrow initial mass range of ∼ 0.1−0.2M⊙ width delineated in Fig.”
- Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, background): “One might argue that, because the disk has a higher overall metallicity than the N-rich sample, the production of N-rich stars is inhibited, because models suggest that intermediatemass AGB stars produce less nitrogen at higher metallicity (Ventura et al. 2013).”
- EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, result): “A similar analysis, but for IMS-AGBs, can be found in Ventura et al. (2013), who compared their models with those published by Karakas (2010), as well as in Fishlock et al. (2014), who made a comparison with a subset of models presented by Straniero et al. (2014).”
- Supermassive stars as a source of abundance anomalies of proton-capture elements in globular clusters (2013, background): “The first is fast rotating massive stars (Decressin et al. 2007) and the second is hot-bottom burning (HBB) in intermediate-mass and massive AGB stars (Dantona et al. 1983; Ventura et al. 2013).”
- 7Li evolution in the thin and thick discs of the Milky Way (2018, background): “We note that in the stellar evolution model considered (Ventura et al. 2013), lithium production can be activated efficiently only in intermediate mass stars (> 3M ), and the possible contribution from extra mixing processes in low mass red giant branch or AGB stars is not included.”
- STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, methodology): “Other stellar evolution codes predict HBB as strong as ours (e.g. Herwig 2004; Weiss & Ferguson 2009; Pignatari et al. 2013) or stronger, in the case of the Full Spectrum of Turbulence models calculated using the ATON code (e.g., Ventura et al. 2013).”
- Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “Indeed, other AGB yield sets are available in the literature, even if most of them are not covering the full range of metallicities and stellar masses needed to properly calculate a GCE model (e.g. Stancliffe et al. 2004; Weiss & Ferguson 2009; Ventura et al. 2013; Battino et al. 2016).”