We present the results of the light curve model fitting technique applied to optical and near-infrared photometric data for a sample of 18 Classical Cepheids ( 11 fundamentals and 7 first overtones ) in the Large Magellanic Cloud ( LMC ) .
We use optical photometry from the OGLE III database and near–infrared photometry obtained by the European Southern Observatory public survey ‘ ‘ VISTA near–infrared survey of the Magellanic Clouds system ’ ’ .
Iso–periodic nonlinear convective model sequences have been computed for each selected Cepheid in order to reproduce the multi–filter light curve amplitudes and shape details .
The inferred individual distances provide an intrinsic weighted mean value for the LMC distance modulus of \mu _ { 0 } = 18.56 mag with a standard deviation of 0.13 mag .
We derive also the Period–Radius , the Period–Luminosity and the Period–Wesenheit relations that are consistent with similar relations in the literature .
The intrinsic masses and luminosities of the best–fitting models show that all the investigated pulsators are brighter than the predictions of the canonical evolutionary mass–luminosity relation , suggesting a significant efficiency of non–canonical phenomena , such as overshooting , mass loss and/or rotation .