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It is well known that the mere location of a Beat Cepheid model in a PeriodRatio \vs Period diagram (Petersen diagram) puts constraints on its metallicityZ. But these bounds are sensitive to the mixture of elements that are lumpedinto the parameter $Z$. In this short paper we update the previous results thatwere based on the Grevesse-Noels solar mixture to the recent, revised Asplund,Grevesse & Sauval (2005) (AGS) solar mixture.  We also examine the effect of the envelope depth on the accuracy of thecomputed pulsation periods. We find that for low period Cepheids with high Zthe customary approximation of envelope pulsation breaks down. It is necessaryto compute stellar models that extend to the center and to include burning andcomposition inhomogeneities in the modeling. Fortunately, however, most BeatCepheids that have been observed so far seem to avoid that regime.

Beat Cepheids as Probes of Stellar and Galactic Metallicity: The New AGS Abundances