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

We present results from a comparative study of light curves of Cepheid and RR\nLyrae stars in the Galaxy and the Magellanic Clouds with their theoretical\nmodels generated from the stellar pulsation codes. Fourier decomposition method\nis used to analyse the theoretical and the observed light curves at multiple\nwavelengths. In case of RR Lyrae stars, the amplitude and Fourier parameters\nfrom the models are consistent with observations in most period bins except for\nlow metal-abundances ($Z<0.004$). In case of Cepheid variables, we observe a\ngreater offset between models and observations for both the amplitude and\nFourier parameters. The theoretical amplitude parameters are typically larger\nthan those from observations, except close to the period of $10$ days. We find\nthat these discrepancies between models and observations can be reduced if a\nhigher convective efficiency is adopted in the pulsation codes. Our results\nsuggest that a quantitative comparison of light curve structure is very useful\nto provide constraints for the input physics to the stellar pulsation models.\n