The characteristics of second-overtone-mode Cepheids predicted by non-linear pulsation models

Details The characteristics of second-overtone-mode Cepheids predicted by non-linear pulsation models The characteristics of second-overtone-mode Cepheids predicted by non-linear pulsation models

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.286l..33a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 286, Issue 3, pp. L33-L37.

Astronomy and Astrophysics

Astronomy

20

Stars: Oscillations, Cepheids

Scientific paper

Non-linear pulsation models of second-overtone-mode Cepheids have been constructed to study the theoretical characteristics of these hypothetical stars which could lead to observational criteria for their identification. The main results of this work are: (1) the light and velocity curves are similar in part to those of first-overtone Cepheid models; (2) the curves are modulated by the resonance between the second- and the sixth-overtone modes, P_2/P_6=2 (3) observed stars should have smaller amplitudes than those of first-overtone s-Cepheids by a factor ~1.6, and should have more symmetric light curves; (4) observed Fourier parameter-period diagrams should be similar to those of first-overtone Cepheids but with the observed resonance `centre' at P~1 d; the true position, however, should be a function of the mass-luminosity relation. Since second-overtone-mode Cepheids may exist in Magellanic Clouds, they could be identified with a certain confidence level by considering their position both in the P-L diagram and in the Fourier parameter diagrams.

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