Stellar Models and Yields of Asymptotic Giant Branch Stars

By A. Karakas, J. Lattanzio. Publications Astronomical Society of Australia, 2007

245 citations recorded by the source corpus.

Abstract We present stellar yields calculated from detailed models of low and intermediate-mass asymptotic giant branch (AGB) stars. We evolve models with a range of mass from 1 to 6 M⊙, and initial metallicities from solar to 1/200th of the solar metallicity. Each model was evolved from the zero age main sequence to near the end of the thermally pulsing (TP) AGB phase, and through all intermediate phases including the core He-flash for stars initially less massive than 2.5 M⊙. For each mass and metallicity, we provide tables containing structural details of the stellar models during the TP-AGB phase, and tables of the stellar yields for 74 species from hydrogen through to sulfur, and for a small number of iron-group nuclei. All tables are available for download. Our results have many applications including use in population synthesis studies and the chemical evolution of galaxies and stellar systems, and for comparison to the composition of AGB and post-AGB stars and planetary nebulae.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/9864a01693596607caa528c5559ea95f02dc1df8

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Citations in the corpus

Abundance patterns of multiple populations in globular clusters: a chemical evolution model based on yields from AGB ejecta (2010, methodology): “This direct correlation is unavoidable, as found in all the relevant AGB computations (Denissenkov & Herwig 2003; Herwig 2004; Karakas & Lattanzio 2007; Ventura & D’Antona 2008b) and as explained in more detail in Section 2.”
The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars (2014, methodology): “…previously that at solar metallicity the maximum mass for the core He flash is 2.1M⊙, whereas at [Fe/H] = −2.3 the maximum mass is 1.75M⊙, with the 2M⊙ model experiencing a fairly quiescent He ignition with only a moderate peak in the He luminosity (Karakas & Lattanzio 2007; Karakas 2010).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “The adoption of the old Karakas & Lattanzio (2007) yields, instead, leads to a huge Na production from LIMSs in the disc (Fig.”
ON THE SOURCE OF THE DUST EXTINCTION IN TYPE Ia SUPERNOVAE AND THE DISCOVERY OF ANOMALOUSLY STRONG Na i ABSORPTION (2013, result): “This is down from the results published in Karakas & Lattanzio (2007), which predict yields of Na that are up to a factor of ≈8 higher (for a 6 M , Z = 0.02 model).”
Origin of multiple stellar populations in globular clusters and their helium enrichment (2008, background): “We encounter here the main difficulty of the AGB scenario, as already pointed out by several authors (e.g. Bekki & Norris 2006; Karakas et al. 2006; Karakas & Lattanzio 2007), that is requiring a first generation of stars much more massive than that still harboured by the cluster.”
A holistic approach to carbon-enhanced metal-poor stars (2009, background): “On the other hand, F is only produced in low-mass AGB stars (see other examples in Karakas & Lattanzio, 2007).”
FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “Variations in the surface luminosityand radius are produced as a consequence of the thermal readjustments taking place during the thermal pulses (see, e.g., Karakas & Lattanzio 2007).”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “25Mg and 26Mg are produced also in He-shell flash convection zone of AGB stars from more massive AGB stars due to α-capture reactions of 22Ne (e.g., Karakas & Lattanzio 2007).”
EVOLUTION, NUCLEOSYNTHESIS, AND YIELDS OF LOW-MASS ASYMPTOTIC GIANT BRANCH STARS AT DIFFERENT METALLICITIES (2009, methodology): “We plot the same quantity for a model computed with an older version of the FRANEC code (Straniero et al. 1997) (hereafter Stra97) and for calculations by other authors (He00; Sta04; Karakas & Lattanzio 2007, hereafter K07).”
Massive AGB models of low metallicity: the implications for the self-enrichment scenario in metal-poor globular clusters (2009, methodology): “We have also computed a set of models with metallicity Z = 10−4, to allow a direct comparison with the metal poor models by Karakas & Lattanzio (2007) and Herwig (2004).”
Evolution of thermally pulsing asymptotic giant branch stars - I. The COLIBRI code (2013, methodology): “The other relation proposed by Straniero et al. (2003), on the basis of their full AGB calculations, appears to be consistent with the Karakas & Lattanzio (2007) results inside its validity range, (i.e. 0.6 .”
Production of dust by massive stars at high redshift (2011, methodology): “Stellar yields for AGB stars have been calculated by e.g., Renzini and Voli (1981),Marigo (2001), Herwig (2004), Karakas and Lattanzio (2007) and recently by Karakas (2010).”
s‐Process in low‐metallicity stars – I. Theoretical predictions (2010, background): “Different evolutionary codes do not reproduce the same results, since they are based on different treatment of the mixing algorithm (see for instance Straniero et al. 2003; Herwig 2004; Karakas & Lattanzio 2007; Stancliffe & Jeffery 2007; Cristallo et al. 2009a, and references therein).”
Young Massive Star Clusters (2010, background): “…massive stars (Prantzos & Charbonnel 2006, Decressin et al. 2007) and massive (4–9 M⊙) Asymptotic Giant Branch (AGB) stars (Ventura et al. 2001, Karakas & Lattanzio 2007 In order to form the large fraction of SG stars suggested by observations (50% or more of the current mass of…”
The evolution of isotope ratios in the Milky Way Galaxy (2011, methodology): “In contrast, Karakas & Lattanzio (2007) adopted initial abundances for the Large and Small Magellanic Clouds from Russell & Dopita (1992) which are sub-solar for C, N, and O.”
The dust content of galaxies from z = 0 to z = 9 (2016, methodology): “We adopt the yields from Karakas & Lattanzio (2007) for low- and intermediate-mass stars (0.8 M/M 8).”
The global gas and dust budget of the Large Magellanic Cloud: AGB stars and supernovae, and the impact on the ISM evolution (2009, background): “Oxygen-rich AGB stars originate both from relatively low mass (1.0–1.5 M ) and relatively high mass (5.0–8.0 M ) stars, at the LMC metallicity (Karakas & Lattanzio 2007).”
Updated stellar yields from asymptotic giant branch models (2009, methodology): “These yields are an update to the results presented in Karakas & Lattanzio (2007), using newer reaction rates and scaled-solar initial abundances for the Z = 0.008 and 0.004 models.”
Yields of AGB and SAGB models with chemistry of low- and high-metallicity globular clusters (2013, result): “These studies complete the previous investigations on these evolutionary phases by Karakas & Lattanzio (2003, 2007), Weiss & Ferguson (2009), and the most recent update by Karakas (2010).”