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The pulsational characteristics of Small Magellanic Cloud Cepheids is examined and compared to the results obtained from linear non-adiabatic models. The possible existence of up to 3 different pulsation modes (fundamental, first and second overtone) is studied and the characteristics, in particular the masses, of the Cepheids which are pulsating under these different modes is presented. The limits of the Cepheid Instability Strip derived from the models for the different modes is also presented and compared with the observed Instability Strip.
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