Abstract
A brief discussion of the physics and numerical techniques for stellar evolution of solar and intermediate-mass stars is followed by a detailed description of the evolution of a \(3\,\mathrm{M}_\odot \) star from the main sequence through the red giant branch, He-core burning, and on to the thermal-pulse AGB evolution. He-shell flashes and the associated mixing as well as the nucleosynthesis are discussed, including the s process. Post-AGB evolution including post-AGB He-shell flashes are presented. Variations of the evolution as a function of mass, the initial–final mass relation, and lifetimes are summarized. Peculiarities of intermediate-mass AGB stars, hot-bottom burning, the super-AGB stars, as well as low-mass stellar evolution through the He-core flash are described in detail. The evolution of low- and intermediate-mass stars is presented. The final chapter covers some aspects of the dynamical star that are not well described in the spherically symmetric framework of stellar evolution.
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Acknowledgments
The author would like to thank the NuGrid collaboration that has enabled the detailed nucleosynthesis simulations discussed in this chapter, and Bill Paxton and the MESA council for creating and supporting the MESA stellar evolution code, as well as Paul Woodward and the members of the LCSE at the University of Minnesota, with whom the author has collaborated substantially to create a new generation of stellar hydrodynamics simulations. The author would like to thank Chris Fryer from Los Alamos National Laboratory and the New Mexico Consortium, Los Alamos, NM for their hospitality during the time when this chapter was finished.
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Herwig, F. (2013). Evolution of Solar and Intermediate-Mass Stars. In: Oswalt, T.D., Barstow, M.A. (eds) Planets, Stars and Stellar Systems. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-5615-1_8
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