Low mass asymptotic giant branch evolution. I

Details Low mass asymptotic giant branch evolution. I Low mass asymptotic giant branch evolution. I

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..821i&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 15, 1982, p. 821-837.

Astronomy and Astrophysics

Astrophysics

123

Asymptotic Giant Branch Stars, Carbon Stars, Giant Stars, Light Curve, M Stars, Stellar Evolution, Stellar Mass, Fine Structure, Late Stars, Stellar Luminosity, Stellar Models, Time Dependence

Scientific paper

Studies of carbon stars and M stars in several external star complexes have demonstrated conclusively that low-mass asymptotic giant branch (AGB) stars of intermediate and low metallicity transform from M stars into C stars. This transformation occurs at a bolometric luminosity brighter than -4. One of the objectives of the present study is to examine theoretical light curves in the small core mass, small M case in more detail than appears in most earlier studies in order to investigate the core mass dependence of the magnitude and duration of the extended luminosity dip which follows a thermal pulse. It is shown that convective dredge-up of carbon to the surface does not occur in standard AGB models of small mass until the core mass approaches a value of approximately 0.7 solar mass. Attention is given to the time dependence of observables for 0.6 solar mass and 0.7 solar mass models, the fine-structure time dependence for the models, and the properties of convective regions.

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