NGC 1866 revisited - Semiconvection versus overshoot

Details NGC 1866 revisited - Semiconvection versus overshoot NGC 1866 revisited - Semiconvection versus overshoot

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...250..340l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 250, no. 2, Oct. 1991, p. 340-350. Research supported by University of Califor

Astronomy and Astrophysics

Astrophysics

18

Color-Magnitude Diagram, Magellanic Clouds, Star Clusters, Stellar Mass, Stellar Models, Charge Coupled Devices, Globular Clusters, Milky Way Galaxy, Open Clusters, Stellar Evolution

Scientific paper

A new set of stellar tracks and related isochrones that take into account the presence of semiconvection in the He-core burning phase is calculated. The stellar masses range from 2.5 to 9 solar masses for two values of the metallicity: Z = 0.02 and Z = 0.003. These models are compared with a set calculated with convective overshoot where the metallicity, the He content and the other parameters are homogeneous. Since the treatment of the convection in the core of a real star is affected by many uncertainties, the observations of the star clusters of the Large Magellanic Cloud are examined to discriminate among semiconvection and overshoot. In particular, the theoretical models are compared with the color-magnitude diagram and the luminosity function of NGC 1866 previously presented by Chiosi et al. (1989). Both models reproduce the features of the color-magnitude diagram; however, only the convective overshoot hypothesis is in agreement with the observed ratio of main sequence to evolved stars.

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