Star clusters of the Large Magellanic Cloud. III - CCD-photometry of NGC 2164

Details Star clusters of the Large Magellanic Cloud. III - CCD-photometry of NGC 2164 Star clusters of the Large Magellanic Cloud. III - CCD-photometry of NGC 2164

Mar 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26as...87..517v&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 87, no. 3, March 1991, p. 517-540. Research supported by Min

Mathematics

Logic

34

Astronomical Photometry, Charge Coupled Devices, Globular Clusters, Magellanic Clouds, Main Sequence Stars, Binary Stars, Color-Magnitude Diagram, Stellar Composition, Stellar Evolution, Stellar Luminosity, Stellar Models, Stellar Spectrophotometry

Scientific paper

The CM diagram and the main-sequence luminosity function (MSLF) of the young globular cluster NGC 2164 are studied in order to discriminate among possible scenarios for the evolution of intermediate-mass stars. BV CCD photometry of stars in the cluster and in a nearby field were obtained. Two main schemes of stellar evolution are tested: (1) the classical models incorporating semiconvection during the He-core burning phase (Lattanzio, 1989) and (2) the models taking into account convective overshoot during both core H- and He-burning phases (Bressan et al., 1981; Bertelli et al., 1985 and 1986). The chemical composition of the stellar content of NGC 2164 turns out to be Z = 0.004 and Y = 0.25. The age of the cluster is 200 Myr for type (2) models and 70 Myr for type (1) models. The comparison of the observational integrated MSLF, normalized to the number of evolved stars, with the theoretical one indicates that type (2) models ought to be preferred.

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