Evolution of massive AGB stars: I.Carbon burning phase

By L. Siess. 2006

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In Astronomy and Astrophysics

Citations in the corpus

Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “Consequently, degeneracy increases in the core, and these stars may undergo thermal pulses (e.g. Iben et al. 1997; Ritossa et al. 1999; Siess 2006) and lose mass as “normal” (but quite massive and luminous) AGBs, the difference being the core composition (O–Ne versus C–”
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.…”
The Evolution of Massive Helium Stars, Including Mass Loss (2019, methodology): “The 1.9 M model was the lowest mass to clearly ignite a sustained carbon CBF (Table 1).”
THE ORBITAL EVOLUTION OF GAS GIANT PLANETS AROUND GIANT STARS (2009, methodology): “These were calculated based on the stellar evolution code STAREVOL described in Siess (2006).”
A NEW CLASS OF LUMINOUS TRANSIENTS AND A FIRST CENSUS OF THEIR MASSIVE STELLAR PROGENITORS (2008, background): “This is traditionally a very difficult phase to model (see the summary in Woosley et al. 2002; Siess 2006; Poelarends et al. 2008).”
Formation and evolution of compact binaries in globular clusters – II. Binaries with neutron stars (2007, background): “As a result, the range varies between different evolutionary codes (see discussion in Podsiadlowski et al. 2004;Siess 2006), and is generally reduced compared to that proposed initially by Nomoto (1984, 1987).”
STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, background): “The 8M models (and the 7M at Z = 0.007) produce a hybrid CO(Ne) core, and experience off-centre carbon flashes but the temperature in the core is not high enough to ignite a carbon flame that reaches the centre (e.g., as described by Siess 2006).”
The Supernova Channel of Super-AGB Stars (2007, methodology): “H and He Core Burning The evolution of stars toward the SAGB has been studied previously (Ritossa et al. 1996, 1999; Iben et al. 1997; GarciaBerro et al. 1997; Siess 2006), and our simulations qualitatively confirm these results, although quantitative differences occur.”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “Whilst this deep dredge-up is not a newly described phenomenon (e.g Becker & Iben 1979; Herwig 2004b; Siess 2006; Lau et al. 2007; Suda & Fujimoto 2010) we have proposed a new nomenclature of “corrosive 2DU” (Gil-Pons et al. 2013; Doherty et al. 2014).”
Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first Super-Earth with measured radius (2009, unknown): “The grid of the STAREVOL stellar evolution models (Siess 2006) was interpolated within the locus defined by the three basic parameters (Teff , M⋆, R⋆) and their associated errors.”
Transiting exoplanets from the CoRoT space mission . VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert (2008, methodology): “In this study, we mainly relied on STAREVOL (Siess 2006; Palacios, private communication) stellar evolution models to derive the stars precise parameters.”
Evolution of massive AGB stars - II. model properties at non-solar metallicity and the fate of Super-AGB stars (2007, methodology): “Details of this evolution as well as of the nucleosynthesis will be provided in a forthcoming paper, however some features can already be anticipated from Siess (2006b, 2007).”
THE REMARKABLE DEATHS OF 9–11 SOLAR MASS STARS (2015, methodology): “…Dominguez et al. (1993); Timmes et al. (1994); Gutierrez et al. (1996); Garcia-Berro et al. (1997); Iben et al. (1997); Ritossa et al. (1999); Siess (2006); Poelarends et al. (2008); Jones et al. (2013); Tauris et al. (2013); Takahashi et al. (2013); Doherty et al. (2014); Jones et al.…”
Stellar Models and Yields of Asymptotic Giant Branch Stars (2007, background): “Yields for these stars should be available in the future (Doherty, Lattanzio & Siess, in preparation), noting that models of these stars are proving to be even more challenging than for CO-core AGB models (Siess 2006).”