On the mass discrepancy of the Cepheid stars

Details On the mass discrepancy of the Cepheid stars On the mass discrepancy of the Cepheid stars

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..205c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Jan. 20, 1992, p. 205-216. Research supported by MURST and ASI.

Astronomy and Astrophysics

Astrophysics

20

Cepheid Variables, Color-Magnitude Diagram, Magellanic Clouds, Open Clusters, Stellar Mass, Stellar Oscillations, Chemical Composition, Milky Way Galaxy, Star Clusters, Stellar Evolution

Scientific paper

The problem of the mass discrepancy of Cepheid stars in the young, rich LMC cluster NGC 2157 observed by Mateo and coworkers, which is known to possess three Cepheids, is presented. The simultaneous fit of the color-magnitude diagram with theoretical simulations based on models for intermediate-mass stars incorporating either semiconvection or overshoot in the central cores, and with suited chemical composition (the evolutionary masses of the Cepheids are therefore automatically known), and the derivation of the pulsational masses from the Cepheid models of Chiosi and Wood (1990) make it possible to show that the problem of mass discrepancy likely originates from the adoption of semiconvective models and insufficient accuracy in the determination of the mass by one of the two methods.

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