Structural Properties of s-Cepheid Velocity Curves

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dc.creatorKienzle, F.
dc.creatorMoskalik, P.
dc.creatorBersier, D.
dc.creatorPont, F.
dc.date1998-07-14
dc.date1998-10-22
dc.date.accessioned2026-07-07T02:27:23Z
dc.date.available2026-07-07T02:27:23Z
dc.descriptionThe 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=2 omega_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. (1999), 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 = 2 omega_1 resonance is estimated to occur at P_r = 4.58+-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.
dc.description8 pages, 6 figures, accepted by Astronomy and Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/9807132
dc.identifierhttp://arxiv.org/abs/astro-ph/9807132
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/12672
dc.subjectAstrophysics
dc.titleStructural Properties of s-Cepheid Velocity Curves
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