1995BaltA...4...39F

The assumption that faint carbon stars in the Magellanic Clouds are on the early asymptotic giant branch (E-AGB) stage is verified using the population simulation technique. We suppose that these stars are formed as a result of the mass transfer in close binary systems, while the primary is a carbon star on the AGB stage. The computed luminosity functions for carbon stars in the E-AGB stage for different initial heavy element abundances and different laws of the mass-loss rate are presented. The expected amount of the E-AGB carbon stars must be comparable with the amount of carbon stars in the thermal-pulsing (TP-AGB) stage. The position of some faint carbon stars of the Magellanic Clouds on the HR diagram is compared with the theoretical E-AGB and TP-AGB tracks.