Structural properties of s-Cepheid velocity curves Constraining the location of the omega_4 = 2omega_1 resonance

Details Structural properties of s-Cepheid velocity curves Constraining the location of the omega_4 = 2omega_1 resonance Structural properties of s-Cepheid velocity curves Constraining the location of the omega_4 = 2omega_1 resonance

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...341..818k&link_type=abstract

Astronomy and Astrophysics, v.341, p.818-826 (1999)

Astronomy and Astrophysics

Astrophysics

27

Techniques: Radial Velocities, Stars: Oscillations, Stars: Variables: Cepheids

Scientific paper

The light curves of the first overtone Pop. I Cepheids (s-Cepheids) show a discontinuity in their phi_ {21} vs. {P} diagram, near {P} = 3.2 day. This feature, commonly attributed to the 2:1 resonance between the first and the fourth overtones (omega_4 ~ 2omega_1 ), is not reproduced by the hydrodynamical models. With the goal of reexamining the resonance hypothesis, we have obtained new CORAVEL radial velocity curves for 14 overtone Cepheids. Together with 10 objects of Krzyt et al. ( te{krzyt}), the combined sample covers the whole range of overtone Cepheid periods. The velocity Fourier parameters display a strong characteristic resonant behavior. In striking contrast to photometric ones, they vary smoothly with the pulsation period and show no jump at 3.2 day. The existing radiative hydrodynamical models match the velocity parameters very well. The center of the omega_4 = 2omega_1 resonance is estimated to occur at {P}r = 4.58\pm 0.04 day, i.e. at a period considerably longer than previously assumed (3.2 day). We identify two new members of the s-Cepheid group: MY Pup and V440 Per. Based on observations collected at the European Southern Observatory (La Silla, Chile) and at the Observatoire de Haute-Provence (France)}

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