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Synthetic AGB Evolution

  • Chapter
Asymptotic Giant Branch Stars

Part of the book series: Astronomy and Astrophysics Library ((AAL))

Abstract

Full stellar evolution calculations are computer-time-consuming, especially when they reach the AGB phase, reflecting the complexity of the inner structure of AGB stars and of the temporal evolution due to thermal pulses (see Chapter 2). Therefore, if one is interested in distribution functions (for example, the luminosity function of AGB stars in a galaxy, or the fraction of AGB stars in a galaxy that are obscured by dust, or population synthesis in general), this is hardly achievable from calculating and integrating over a set of tens to hundreds of full stellar evolutionary models. In addition, full stellar models depend critically on a number of uncertain parameters, like mass loss, mixing length, and convective dredge-up of nucleosynthesis products. Clearly, it is computationally prohibitive to calculate a grid of stellar evolution models (including the AGB phase) sufficiently spaced in mass, and for different choices of initial metallicities, mass loss, and other parameters.

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Authors and Affiliations

  1. Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium

    Martin A. T. Groenewegen

  2. Department of Astronomy, University of Padova, Italy

    Paula Marigo

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  1. Martin A. T. Groenewegen
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  2. Paula Marigo
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  1. Leiden Observatory, University of Leiden, 2300 RA, Leiden, The Netherlands

    Harm J. Habing

  2. Stockholm Observatory, Stockholm University, Alba Nova, SE-10691, Stockholm, Sweden

    Hans Olofsson

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Groenewegen, M.A.T., Marigo, P. (2004). Synthetic AGB Evolution. In: Habing, H.J., Olofsson, H. (eds) Asymptotic Giant Branch Stars. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4757-3876-6_3

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