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- W2000731521 abstract "view Abstract Citations (8) References (28) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Termination of Shell Burning of Helium in Solar-Mass Stars Kutter, G. S. Abstract The evolution of a 1.04 o star, composed initially of a 1 M0 12C core and a 0.04 M0 4He-rich envelope, is followed through the termina] phase of 4He shell burning to the white-dwarf stage. During the phase of maximum 4He burning, the phofon luminosity (-- 10 6L0) exceeds by a factor of 2 the critical luminosity above which mass loss occurs by momentum transfer from the radiation to the gas. This represents a possible mechanism for the ejection of planetary nebulae from highly evolved stars in the approximate range 1 0-1.4 . Qualitative agreement with the observational data of the precursor stars and the nuclei of planetary nebulae tends to support this connection. Helium shell burning is extinguished when the time scale of photon diffusion from the shell source to the surface becomes of the order of the time scale of nuclear energy production, u/ ( [3a + tt12C(a, )16O] the shell source loses energy more rapidly than it can replenish by nuclear burning and contraction. No thermal instabilities have been found, probably because of the large contribution of radiation to the equation of state in and above the shell source (0.30 < p < 0.65). Publication: The Astrophysical Journal Pub Date: February 1971 DOI: 10.1086/150822 Bibcode: 1971ApJ...164..115K full text sources ADS |" @default.
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- W2000731521 date "1971-02-01" @default.
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- W2000731521 title "Termination of Shell Burning of Helium in Solar-Mass Stars" @default.
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