High-luminosity carbon stars in the early asymptotic giant branch phase

Details High-luminosity carbon stars in the early asymptotic giant branch phase High-luminosity carbon stars in the early asymptotic giant branch phase

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995azh....72..841f&link_type=abstract

Astronomicheskij Zhurnal, vol. 72, p. 841

Astronomy and Astrophysics

Astronomy

2

Carbon Stars, Stellar Luminosity, Asymptotic Giant Branch Stars, Magellanic Clouds, Stellar Temperature, Stellar Evolution, Mass Transfer, Binary Stars, Stellar Atmospheres

Scientific paper

There are high-luminosity carbon stars in the Large Magellanic Cloud (LMC) whose effective temperatures are well above those of ordinary N-type stars. To elucidate the evolutionary stage of these stars, the populations of carbon stars formed as a result of both single-star evolution and mass transfer in close binary systems have been theoretically modeled by the method of synthetic evolution. It is shown that high-luminosity carbon stars in the LMC with effective temperatures greater than those of most of the LMC stars are in the early asymptotic giant branch (AGB) phase, while most of the carbon stars with significantly lower effective temperatures are in the phase of helium-shell flashes. This conclusion is confirmed by the observation of carbon and S-type LMC stars in clusters where these stars are clearly separated into two groups according to their effective temperature. It appears that such stars cannot be present in the Galaxy because of large heavy-element abundances, intermediate-mass stars in the early AGB phase do not reach high luminosities.

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