Abstract
In the preceding chapter we have seen how one can compute the evolution of a star by starting from a homogeneous model representing a newly formed system. When the chemical composition of the star changes with time, a new model is computed each time. In this chapter we shall consider the theoretical evolutionary paths of systems with various masses and see how the computed evolution explains the observational data. The following discussion is rather qualitative, since the details of the theoretical calculations are too involved for the present book.
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Further Reading
Bowers, Deeming: Astrophysics I: Stars, Jones and Bartlett Publishers 1984.
Böhm-Vitense: Introduction to Stellar Astrophysics; Cambridge University Press, Vol. 1–3 1989–1992.
Clayton: Principles of Stellar Evolution and Nucleosynthesis,McGraw-Hill 1968.
Hansen, Kawaler: Stellar interiors, Physical principles, structure and evolution, Springer 1994.
Harpaz: Stellar Evolution,Peters Wellesley 1994.
Kippenhahn, Weigert: Stellar Structure and Evolution, Springer, 2nd ed. 1994.
Phillips: The physics of Stars,Manchester Phys. Ser. 1994, 2nd ed. 1999.
Taylor: The Stars: their structure and evolution,Cambridge University Press 1994.
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Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (2003). Stellar Evolution. In: Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (eds) Fundamental Astronomy. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-05333-1_11
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DOI: https://doi.org/10.1007/978-3-662-05333-1_11
Publisher Name: Springer, Berlin, Heidelberg
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