Beat Cepheid Period Ratios from OPAL Opacities

Abstract

The discovery of a large number of beat Cepheids in the Large Magellanic Cloud in the MACHO survey, provides an opportunity to compare the characteristics of such Cepheids over a range of metallicities. We produced a large grid of linear nonadiabatic pulsation models using the OPAL opacity tables and with compositions corresponding to those of the Milky Way, and the Large and Small Magellanic Clouds. Using the relationship between the period ratio and the main pulsation period, we are able to define a range of models which correspond to the observed beat Cepheids, and thereby constrain the physical characteristics of the LMC beat Cepheids. We are also able to make some predictions about the nature of the yet-to-be-discovered SMC beat Cepheids.

20 pages, 6 embedded Postscript figures, uses aasms4.sty. Accepted for publication in the 1997 September AJ

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• New homogeneous iron abundances of double-mode Cepheids from high-resolution echelle spectroscopy
• Beat Cepheids as Probes of Stellar and Galactic Metallicity
• Cepheid models based on self-consistent stellar evolution and pulsation calculations: the right answer?
• The triple-mode pulsating variable V823 Cas
• HD 304373, the second case of 1O/2O double-mode Cepheid in the Galaxy
• The contribution of microlensing surveys to the distance scale