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We study in depth the abundance discrepancy problem in H II regions, thistime from a different perspective than the usual one: by studying the effect ofthe upper mass limit (M$_{\rm up}$) of the initial mass function (IMF) on theO, C, and He predicted by chemical evolution models for the Milky Way. We useabundances determined with the direct method (DM) and with the temperatureindependent method (TIM). We compare the predicted abundances at the presenttime with observations of Orion, M17, and M8 to determine the M$_{\rm up}$value of the galactic IMF. From the DM abundances, the models predict anM$_{\rm up}$ = 25-45 M$_{\odot}$, while from the TIM, CEMs derive an M$_{\rmup}$ = 70-110 M$_{\odot}$. Spiral galaxies with the stellar mass and starformation rate of the MW are predicted to have an M$_{\rm up} \sim100$M$_{\odot}$. These results support that abundances derived from the TIM arebetter than those derived from the DM.

The ADF and the t$^2$ formalism in H II regions based on the upper mass limit of the IMF for the MW