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The Geneva stellar evolution code

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Abstract

This paper presents the Geneva stellar evolution code with special emphasis on the modeling of solar-type stars. The basic input physics used in the Geneva code as well as the modeling of atomic diffusion is first discussed. The physical description of rotation is then presented. Finally, the modeling of magnetic instabilities and transport of angular momentum by internal gravity waves is briefly summarized.

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  1. P. Eggenberger

    Present address: Institut d’Astrophysique et de Géophysique, l’Université de Liège, Allée du 6 Août 17, 4000, Liège, Belgium

Authors and Affiliations

  1. Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290, Sauverny, Switzerland

    P. Eggenberger, G. Meynet, A. Maeder, C. Charbonnel & S. Ekström

  2. Department of Physics and Astronomy, University of Basel, Klingelbergstr. 82, 4052, Basel, Switzerland

    R. Hirschi

  3. Laboratoire d’Astrophysique de l’OMP, CNRS UMR 5572, 31400, Toulouse, France

    C. Charbonnel

  4. Departement de Physique, Université de Montréal, Montréal, PQ H3C 3J7, Canada

    S. Talon

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  1. P. Eggenberger
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Eggenberger, P., Meynet, G., Maeder, A. et al. The Geneva stellar evolution code. Astrophys Space Sci 316, 43–54 (2008). https://doi.org/10.1007/s10509-007-9511-y

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