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The Structure and Evolution of Massive Stars

Published online by Cambridge University Press:  14 August 2015

C. Chiosi
C. Chiosi*
Affiliation:
Instituto di Astronomia, Universita di Padova

Extract

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This review is restricted to the most recent studies of the structure of stars in the approximate range from 10 to 100 M⊙, during the core H- and He-burning phases. Other recent major reviews on this subject are by Dallaporta (1971), Massevich and Tutukov (1974) and Iben (1974). The lower limit was chosen to be just above the transition from degeneracy to non-degeneracy in the core at carbon ignition (Schwarzschild and Härm 1958). The upper limit is very uncertain. The canonical value of about 60 M⊙ for Pop I composition was set by Schwarzschild and Harm (1959), using linear pulsation theory. More recent non-linear dynamical calculations lift the limit above 100 M⊙, and also show that mass loss by vibrational instability occurs at such a rate that stars in the range from 100 to 200 M⊙ can survive for a time comparable to the total main sequence lifetime (Appenzeller 1970a, b, Ziebarth 1970, Talbot 1971a,b and Papaloizou and Taylor 1974).

Type
Part VII: Theoretical Papers and Summary
Information
Symposium - International Astronomical Union , Volume 80: The HR Diagram , 1978 , pp. 357 - 368
Copyright
Copyright © Reidel 1978 

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