Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..671b&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 671-679.
Astronomy and Astrophysics
Astrophysics
111
Carbon Stars, Metallicity, Stellar Evolution, Stellar Interiors, Stellar Mass, Nuclear Reactions, Stellar Cores, Stellar Envelopes, Stellar Luminosity, Stellar Winds
Scientific paper
Detailed stellar evolutionary calculations were carried out for a metal-poor case (Z = 0.001) for stars of initial masses 1.0 M_sun;, 1.2 M_sun;, 2.0 M_sun;, and 3.0 M_sun;, and for a metal-rich case (Z = 0.02) for stars of initial masses 1.2 M_sun; and 3.0 M_sun;. Ongoing mass loss via a Reimers-type wind was included. The stars were evolved from the main sequence through all intermediate stages and finally through a number of helium shell flashes (thermal pulses) on the asymptotic giant branch. Classical "third dredge-up" and carbon star production were obtained in two cases, both having metallicity Z = 0.001. A 1.72 M_sun; star (of initial mass 2.0 M_sun;) whose mixing length parameter had been increased to α = 1.5 became a carbon star on its 11th flash, with a core mass of 0.665 M_sun;. A 0.81 M_sun; star (of initial mass 1.2 M_sun;) became a carbon star immediately after its mixing length parameter was increased to α = 3.0, on its sixth flash, with a core mass of 0.566 M_sun;.
Boothroyd Arnold I.
Sackmann I.-Juliana
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