BL Herculis stars - Theoretical models for field variables

Details BL Herculis stars - Theoretical models for field variables BL Herculis stars - Theoretical models for field variables

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..740c&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 15, 1982, p. 740-748. Research supported by the Science Research Council of Engla

Astronomy and Astrophysics

Astrophysics

20

Cepheid Variables, Light Curve, Metallic Stars, Stellar Evolution, Stellar Luminosity, Stellar Models, Chemical Composition, Globular Clusters, Hertzsprung-Russell Diagram

Scientific paper

Type II Cepheids with periods between 1 and 3 days, commonly designated as Bl Herculis stars, have been modeled here with the aim of interpreting the wide variety of light curves observed among the field variables. Previously modeled globular cluster members are used as standard calibration objects. The major finding is that only a small range of luminosities is capable of generating a large variety of light curve types at a given period. For a mass of approximately 0.60 solar mass, the models are able to reproduce the observed mean luminosities, dispersion of mean luminosities, periods, light amplitudes, light asymmetries, and phases of secondary features in the light curves of known BL Her stars. It is possible that the metal-rich variables (which are found only in the field) have luminosities lower than those of most metal-poor variables. The present revised mass for BL Her, a metal-rich object, is not significantly different from the mean mass of the metal-poor variables.

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