On the evolution of massive stars through the core carbon-burning phase

Details On the evolution of massive stars through the core carbon-burning phase On the evolution of massive stars through the core carbon-burning phase

Jul 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...207..209l&link_type=abstract

Astrophysical Journal, vol. 207, July 1, 1976, pt. 1, p. 209-232.

Statistics

Computation

115

Carbon Stars, Main Sequence Stars, Stellar Evolution, Stellar Mass, Stellar Models, Supergiant Stars, Chemical Composition, Interstellar Radiation, Nitrogen Isotopes, Spectrum Analysis, Stellar Envelopes, Stellar Luminosity, Stellar Temperature, Time Dependence

Scientific paper

Results are presented for detailed calculations of the evolution of model stars with Population I compositions and masses of 15 and 25 solar masses from the main-sequence phase to the core carbon-burning phase. Up to 1100 mass shells, a full reaction network in the later stages of evolution, and energy losses due to a direct electron-neutrino interaction are included in the computations. Those results which have a bearing on the observable properties of massive stars include the following: (1) objects near 15 solar masses will ignite and burn carbon as red supergiants, but objects as massive as 25 solar masses will ignite carbon in a region considerably to the blue of the red-supergiant branch; (2) there are effective upper limits to the mass and period of classical Cepheids which are determined by the intersection in the H-R diagram of a core carbon-burning band and a theoretical pulsational-instability strip; (3) stars near 15 solar masses will experience enhancement in surface abundance of hydrogen-burning products toward the end of their redward transit of the Hertzsprung gap at the end of core helium burning; and (4) stars of 25 solar masses will develop such enhancement, if at all, only after their evolution has become so rapid as to render them unobservable.

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