Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..175r&link_type=abstract
Astronomy and Astrophysics, vol. 94, no. 1, Jan. 1981, p. 175-193. Research supported by the Consiglio Nazionale delle Ricerche
Astronomy and Astrophysics
Astrophysics
859
Abundance, Carbon Stars, Nuclear Fusion, Planetary Nebulae, Stellar Evolution, Stellar Mass Ejection, Elliptical Galaxies, Helium, Magellanic Clouds, Main Sequence Stars, Milky Way Galaxy, Red Giant Stars, Stellar Envelopes, Stellar Mass, Stellar Winds
Scientific paper
The evolution of the surface abundances of He-4, C-12, C-13, N-14, and O-16, in intermediate-mass stars (1-8 solar masses) have been computed from the main-sequence phase, till the ejection of the envelope (planetary-nebula ejection), or until the carbon ignition in the core. Two processes affecting the surface composition have been taken into account, namely: (1) convective dredge-ups, and (2) nuclear burning in the deepest layers of the convective envelope. Mass loss due to the stellar wind in the red-giant phase, and the envelope ejection leading to the formation of planetary nebulae have been also taken into account. In this way, several individual and collective properties of carbon stars are predicted, as well as the expected compositions of planetary nebulae, and the contribution of intermediate-mass stars to the galactic nucleosynthesis of the nuclides listed above. The primary production of C-13 and N-14 is also treated. A preliminary comparison with the observations shows that the present theory is able to account for several characteristics of carbon stars in the Galaxy, as well as in the Magellanic Clouds, and in the dwarf elliptical galaxy in Fornax. The theory accounts also for the observed range of helium abundances in planetary nebulae.
Renzini Alvio
Voli Marco
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