I investigate the discrepancy between the evolution and pulsation masses for Cepheid variables .
A number of recent works have proposed that non-canonical mass-loss can account for the mass discrepancy .
This mass-loss would be such that a 5 M _ { \odot } star loses approximately 20 % of its mass by arriving at the Cepheid instability strip ; a 14 M _ { \odot } star , none .
Such findings would pose a serious challenge to our understanding of mass-loss .
I revisit these results in light of the Padova stellar evolutionary models and find evolutionary masses are ( 17 \pm 5 ) % greater than pulsation masses for Cepheids between 5 < M / M _ { \odot } < 14 .
I find that mild internal mixing in the main-sequence progenitor of the Cepheid are able to account for this mass discrepancy .