Evolution of massive AGB stars - III. the thermally pulsing super-AGB phase

By L. Siess. 2010

135 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/75af6a8170c5b3a9a2840b3a4f5c34a2dc5217c4

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In Astronomy and Astrophysics

1. A. Karakas
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Citations in the corpus

• Pulsating white dwarfs: new insights (2019, methodology): “In fact, on the one hand, the heaviest intermediate mass stars (Mi ∼> 8M⊙) might reach temperatures in the core high enough to ignite C, enter the Super-AGB phase and end up as oxygen/neon (ONe)-core WDs (Ritossa et al., 1996; Siess, 2010)9.”
• Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, background): “These stars are expected to evolve through a short-lived super-AGB phase (e.g. Siess 2010), and will not be considered in this paper.”
• Evolution of thermally pulsing asymptotic giant branch stars - I. The COLIBRI code (2013, background): “In a recent study Siess (2010) reported that ≈ 6 months of CPU time were required by his full evolution code to follow the whole Super-AGB phase of just one model with strong HBB.”
• Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “Here, M up,Ne ∼ 9 ± 1 M is the upper mass limit of the progenitor of an O+Ne+Mg white dwarf and is smaller for lower metallicities (Siess 2007, 2010; Poelarends et al. 2008; Pumo et al. 2009; Langer 2012).”
• 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).”
• NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, methodology): “For super-AGB stars one may use the models of Siess (2010) which do not include heavy elements.”
• Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “In computations of super-AGB stars the efficiency of 3DU ranges from: no 3DU (λ=0) as found by Siess (2010) and Ventura et al. (2013); slight 3DU (λ ∼ 0.07− 0.30) found by Ritossa et al. (1996); efficient 3DU (λ ∼ 0.4 − 0.8) found in this work and Gil-Pons et al. (2013); or extreme 3DU (λ≈1) found…”
• Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, methodology): “Because of the smaller mass loss experienced, the yields by Siess (2010) are more Mg–poor, because there is more time available to destroy the surface magnesium via HBB.”
• SURVEYING THE AGENTS OF GALAXY EVOLUTION IN THE TIDALLY STRIPPED, LOW METALLICITY SMALL MAGELLANIC CLOUD (SAGE-SMC). II. COOL EVOLVED STARS (2011, background): “These stars undergo efficient hot bottom burning (HBB; Smith & Lambert 1985; Boothroyd & Sackmann 1992) and are expected to suffer from weak thermal pulses, reach lower temperatures, and achieve higher mass-loss rates than their lower-mass cousins (Siess 2010).”