2000ApJ...544.1056F

A hydrodynamical survey of the pulsational properties of first-overtone Galactic Cepheids is presented. The goal of this study is to reproduce their observed light and radial velocity curves. The comparison between the models and the observations is made in a quantitative manner on the level of the Fourier coefficients. Purely radiative models fail to reproduce the observed features, but convective models give good agreement. It is found that the sharp features in the Fourier coefficients are indeed caused by the P₁/P₄=2 resonance, despite the very large damping of the fourth overtone. For the adopted mass-luminosity relation, the resonance center lies near a period of 4{fd}2±0{fd}3 as indicated by the observed radial velocity data rather than near 3{fd}2 as the light curves suggest.