We present the results of a theoretical investigation aimed at testing whether full amplitude , nonlinear , convective models account for the I-band light curves of Bump Cepheids in the Large Magellanic Cloud ( LMC ) .
We selected two objects from the OGLE sample that show a well-defined bump along the decreasing ( short-period ) and the rising ( long-period ) branch respectively .
We find that current models do reproduce the luminosity variation over the entire pulsation cycle if the adopted stellar mass is roughly 15 % smaller than predicted by evolutionary models that neglect both mass loss and convective core overshooting .
Moreover , we find that the fit to the light curve of the long-period Cepheid located close to the cool edge of the instability strip requires an increase in the mixing length from 1.5 to 1.8 Hp .
This suggests an increase in the efficiency of the convective transport when moving toward cooler effective temperatures .
Current pulsation calculations supply a LMC distance modulus ranging from 18.48 to 18.58 mag .