A comparison of observed and theoretical luminosity functions of carbon stars and late M giants

Details A comparison of observed and theoretical luminosity functions of carbon stars and late M giants A comparison of observed and theoretical luminosity functions of carbon stars and late M giants

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..259m&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 259-268. Research supported by the Alfred P. Sloan Foundation

Astronomy and Astrophysics

Astrophysics

19

Carbon Stars, Giant Stars, Late Stars, M Stars, Stellar Luminosity, Abundance, Computerized Simulation, Metals, Milky Way Galaxy, Stellar Models, Stellar Structure

Scientific paper

Simulated populations of double-shell phase stellar models undergoing mixing due to helium shell flashes are compared with observations of carbon stars and M giants in the Galaxy, the LMC, the SMC, and the Fornax dwarf galaxy. The available observational constraints for C stars and late M giants in these objects is summarized, and the simulation technique and parametrized mixing model employed is briefly described. The main parameters for which simulation results are obtained are the metal abundance, the fraction of intershell carbon mixed up per flash, the minimum core mass at which mixing begins, the core mass above which mixing does not occur, and the duration of star formation. It is found that the observed variation of the C/M ratio with metal abundance can be accounted for in just about any model for mixing, nearly independently of parameters. The observed C/M variation is, however, a potential probe of metal abundances and their spatial variation in nearby galaxies.

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