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.
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Further Reading
Clayton, D. D. (1968/1983): Principles of Stellar Evolution and Nucleosynthesis (McGraw-Hill, New York/University of Chicago Press, Chicago)
Novotny, E. (1973): Introduction to Stellar Atmospheres and Interiors (Oxford University Press, New York).
Schwarzschild, M. (1958/1965): Structure and Evolution of the Stars (Princeton University Press, Princeton/Dover, New York)
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© 1996 Springer-Verlag Berlin Heidelberg
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Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (1996). Stellar Evolution. In: Karttunen, H., Kröger, P., Oja, H., Poutanen, M., Donner, K.J. (eds) Fundamental Astronomy. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-03215-2_12
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DOI: https://doi.org/10.1007/978-3-662-03215-2_12
Publisher Name: Springer, Berlin, Heidelberg
Print ISBN: 978-3-540-60936-0
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