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We present the study of the metallicity dependence of the Fourier amplituderatios R_21 and R_31 for the light curves of short-period Galactic classicalCepheids in B, V, R_C and I_C bands. Based on the available photometric andspectroscopic data we determined the relations between the atmospheric ironabundance, [Fe/H], and the Fourier parameters. Using these relations wecalculated the photometric [Fe/H] values of all program Cepheids with anaverage accuracy of 0.15 dex. No spectroscopic iron abundance was known beforefor 14 of these stars. These empirical results provide an alternate method todetermine the iron abundance of classical Cepheids too faint for spectroscopicobservations. We also checked whether the metal-poor Cepheids of bothMagellanic Clouds follow the same relationships, and a good agreement wasfound.

Determination of the iron content of Cepheids from the shape of their light curves