Stellar evolution in blue populous clusters of the Small Magellanic Cloud and the problems of envelope semiconvection and convective core overshooting

Details Stellar evolution in blue populous clusters of the Small Magellanic Cloud and the problems of envelope semiconvection and convective core overshooting Stellar evolution in blue populous clusters of the Small Magellanic Cloud and the problems of envelope semiconvection and convective core overshooting

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...390..136s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 390, no. 1, May 1, 1992, p. 136-143.

Astronomy and Astrophysics

Astrophysics

82

Convection, Magellanic Clouds, Open Clusters, Star Clusters, Stellar Cores, Stellar Evolution, Chemical Composition, Hertzsprung-Russell Diagram, Stellar Mass, Stellar Structure, Supergiant Stars

Scientific paper

New theoretical evolutionary sequences of models for stars with low metallicities, appropriate to the Small Magellanic Cloud, are derived with both standard Cox-Stewart opacities and the new Rogers-Iglesias opacities. Only those sequences with little or no convective core overshooting are found to be capable of reproducing the two most critical observations: the maximum effective temperature displayed by the hot evolved stars and the difference between the average bolometric magnitudes of the hot and cool evolved stars. An upper limit to the ratio of the mean overshoot distance beyond the classical Schwarzschild core boundary to the local pressure scale height is set at 0.2. It is inferred from the frequency of cool supergiants in NGC 330 that the Ledoux criterion, rather than the Schwarzschild criterion, for convection and semiconvection in the envelopes of massive stars is strongly favored. Residuals from the fitting for NGC 330 suggest the possibility of fast interior rotation in the stars of this cluster. NGC 330 and NGC 458 have ages of about 3 x 10 exp 7 and about 1 x 10 exp 8 yr, respectively.

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