The Dawes Review 2: Nucleosynthesis and Stellar Yields of Low- and Intermediate-Mass Single Stars

By A. Karakas, J. Lattanzio. Publications Astronomical Society of Australia, 2014

499 citations recorded by the source corpus.

Abstract The chemical evolution of the Universe is governed by the chemical yields from stars, which in turn are determined primarily by the initial stellar mass. Even stars as low as 0.9 M⊙ can, at low metallicity, contribute to the chemical evolution of elements. Stars less massive than about 10 M⊙ experience recurrent mixing events that can significantly change the surface composition of the envelope, with observed enrichments in carbon, nitrogen, fluorine, and heavy elements synthesized by the slow neutron capture process (the s-process). Low- and intermediate-mass stars release their nucleosynthesis products through stellar outflows or winds, in contrast to massive stars that explode as core-collapse supernovae. Here we review the stellar evolution and nucleosynthesis for single stars up to ~ 10 M⊙ from the main sequence through to the tip of the asymptotic giant branch (AGB). We include a discussion of the main uncertainties that affect theoretical calculations and review the latest observational data, which are used to constrain uncertain details of the stellar models. We finish with a review of the stellar yields available for stars less massive than about 10 M⊙ and discuss efforts by various groups to address these issues and provide homogeneous yields for low- and intermediate-mass stars covering a broad range of metallicities.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d1afb09ba16921eec206de89004f2f3959c0ebd5

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In Astronomy and Astrophysics

1. A. Karakas
2. Timothy C. Beers
3. M. Lugaro
4. Hans-Walter Rix
5. Jo Bovy
6. C. Sneden
7. I. Minchev
8. S. Majewski

In Instrumentation

1. M. Lugaro
2. A. Karakas
3. C. Sneden
4. Timothy C. Beers
5. J. Cowan
6. S. Majewski
7. J. E. Lawler
8. C. Allende Prieto

Citations in the corpus

• Chemical tagging with APOGEE: Discovery of a large population of N-rich stars in the inner Galaxy (2016, background): “…000, 2–27 posed involve stellar rotation, thermohaline mixing, magnetic fields, meridional circulation combined with turbulent diffusion, or perhaps some combination of some of these processes (e.g., Renzini & Voli 1981; Charbonnel & Lagarde 2010; Angelou et al. 2012; Karakas & Lattanzio 2014).”
• 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): “The interested reader can find a vast literature on AGB stars (Iben & Renzini 1983; Herwig 2005; Straniero et al. 2006; Karakas & Lattanzio 2014).”
• Red giant masses and ages derived from carbon and nitrogen abundances (2015, unknown): “…helium fraction and abundance in α elements also influence the depth reached by the envelope because they impact its opacity (Sweigart, Greggio, & Renzini 1989; Boothroyd & Sackmann 1999), but these are only minor effects for stars below 3 M (cid:2) (Charbonnel 1994; Karakas & Lattanzio 2014).”
• Mass loss of stars on the asymptotic giant branch (2018, background): “Nucleosynthesis and stellar yields of single AGB stars are the topic of a recent review by Karakas and Lattanzio (2014), while binary evolution is discussed by De Marco and Izzard (2017).”
• Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, background): “In particular it depends dramatically on the treatment of the coupling between burning and mixing, mass-loss rate etc therefore, theoretical yields in this mass range are very uncertain (see e.g. Karakas & Lattanzio 2014, and references therein).”
• STELLAR YIELDS FROM METAL-RICH ASYMPTOTIC GIANT BRANCH MODELS (2016, methodology): “1 from Karakas & Lattanzio 2014).”
• Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “For many of these nuclei experimental data are available (see e.g. Käppeler et al., 2011; Karakas and Lattanzio, 2014; Reifarth et al., 2014).”