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We present results from a comparative study of light curves of Cepheid and RRLyrae stars in the Galaxy and the Magellanic Clouds with their theoreticalmodels generated from the stellar pulsation codes. Fourier decomposition methodis used to analyse the theoretical and the observed light curves at multiplewavelengths. In case of RR Lyrae stars, the amplitude and Fourier parametersfrom the models are consistent with observations in most period bins except forlow metal-abundances ($Z<0.004$). In case of Cepheid variables, we observe agreater offset between models and observations for both the amplitude andFourier parameters. The theoretical amplitude parameters are typically largerthan those from observations, except close to the period of $10$ days. We findthat these discrepancies between models and observations can be reduced if ahigher convective efficiency is adopted in the pulsation codes. Our resultssuggest that a quantitative comparison of light curve structure is very usefulto provide constraints for the input physics to the stellar pulsation models.

Light Curve Parameters of Cepheid and RR Lyrae Variables at Multiple Wavelengths $-$ Models vs. Observations