Evolution of massive AGB stars - II. model properties at non-solar metallicity and the fate of Super-AGB stars

By L. Siess. 2007

207 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d365fefc8f6519db94702079d88997c144294a7d

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Citations in the corpus

Production of dust by massive stars at high redshift (2011, background): “Siess (2007, 2008) showed that at very low metallicity (Z = 10−6), the mass range for stars becoming an ECSN is much broader (7.6–9.8 M⊙).”
Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, methodology): “On the side of SAGB modeling, the recent works by Siess (2006, 2007, 2010) provided a complete and exhaustive update of the pioneering explorations focused on the physics of carbon ignition in regime of partial degeneracy, by Ritossa et al. (1996, 1999), Garcia Berro et al. (1997), Iben et al.…”
Evolutionary and pulsational properties of white dwarf stars (2010, background): “It is now accepted that white dwarfs constitute the end-product of all stars with initial masses up to∼ 11M⊙ (Siess 2007).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, background): “This mass interval is the domain of the so-called super-AGB stars, that have not reliable nucleosynthetic utput (Siess 2007; Pumo et al. 2008, and references therein).”
Multiple populations in globular clusters (2012, background): “…the blue MS of ω Cen and NGC 2808 (Bedin et al. 2004; Norris 2004; Piotto et al. 2005; D’Antona et al. 2005; Piotto et al. 2007), it is difficult to produce Y > 0.35 with AGB stars, although values up to Y ∼ 0.38 can be possibly produced by super-AGB stars (Siess 2007; Ventura & D’Antona 2011).”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “Simulations for super-AGB stars (e.g., Siess 2007; Poelarends et al. 2008; Doherty et al. 2010; Ventura & D’Antona 2011), electron-capture SN (e.g., Nomoto 1984; Hoffman et al. 2008; Wanajo – 5 – et al. 2009), SNIa (e.g., Hillebrandt & Niemeyer 2000) and r process (Thielemann et al. 2011) are not…”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “The upper limit of AGB stars, Mu,1, is defined as the minimum mass for carbon ignition, and is estimated to be larger at high metallicity and also at low metallicity than at Z ∼ 10−4 (Gil-Pons et al. 2007; Siess 2007).”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, methodology): “…et al. (2008) whilst an overview for their entire metallicity range provided in fig.12 in Langer (2012) 11 There is a a typographically error in Siess (2007) pg.905, where the Ṁenv should be 5×10−5 M⊙ yr−1 instead of 5×10−4 M⊙ yr−1. growth rate taken from detailed models and parameterised…”
The Origin of Elements from Carbon to Uranium (2020, background): “The upper limit of AGB stars, Mup,C, is defined as the minimum mass for carbon ignition, and is estimated to be larger at high metallicity and also for metallicities lower than Z∼10−4 (Gil-Pons et al. 2007; Siess 2007).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “1 M⊙ or ∼ 4% of all supernovae, Siess 2007; Poelarends et al. 2008) leads to the explosion channel, although the range could be wider for lower metallicity stars.”
EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF AGB STARS AT DIFFERENT METALLICITIES. III. INTERMEDIATE-MASS MODELS, REVISED LOW-MASS MODELS, AND THE pH-FRUITY INTERFACE (2015, background): “Note that there are other published papers on IMS-AGBs; however, they concentrate on different mass regimes (e.g. Siess 2007; Doherty et al. 2015) or present sets for a single metallicity(Herwig 2004).”
Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, methodology): “2.1, super-AGBs may play an important role in the evolution of proto–GCs. Siess (2007a) shows that their helium content in the envelope may reach the values Y=0.36 – 0.38, reasonably consistent with the highest helium content found in the extreme populations of a few GCs, and Pumo et al. (2008)…”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “The upper limit of AGB stars, M up,C, defined here as the minimum mass for the off-center C ignition to occur, is smaller for lower metallicity (Umeda et al. 1999; Gil-Pons, Gutiérrez & Garcı́a-Berro 2007; Siess 2007).”
SN 2008S: An electron-capture SN from a super-AGB progenitor? (2009, background): “Nomoto (1984, 1987) estimated that stars with a mass of 8– c© 0000 RAS, MNRAS000, 000–000 10 M⊙ can become ECSNe but recent work has suggested a more narrow mass range (Siess 2007; Poelarends et al. 2008) and a lower mass limit of∼9 M⊙.”
Abundance patterns of multiple populations in globular clusters: a chemical evolution model based on yields from AGB ejecta (2010, methodology): “Pumo et al. (2008) noticed that a very high helium content (Y up to ∼0.38) can be achieved already just after the second dredge–up in the envelopes of the most massive super–AGB’ stars, as shown by the models by Siess (2007a).”