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We present and discuss results from chemical evolution models for M33. Forour models we adopt a galactic formation with an inside-out scenario. Themodels are built to reproduce three observational constraints of the M33 disk:the radial distributions of the total baryonic mass, the gas mass, and the O/Habundance. From observations, we find that the total baryonic mass profile inM33 has a double exponential behavior, decreasing exponentially for r<= 6 kpc,and increasing lightly for r > 6 kpc due to the increase of the gas masssurface density. To adopt a concordant set of stellar and H II regions O/Hvalues, we had to correct the latter for the effect of temperature variationsand O dust depletion. Our best model shows a good agreement with the observedthe radial distributions of: the SFR, the stellar mass, C/H, N/H, Ne/H, Mg/H,Si/H, P/H, S/H, Ar/H, Fe/H,and Z. According to our model, the star formationefficiency is constant in time and space for r <= 6 kpc, but the SFR efficiencydecreases with time and galactocentric distance for r > 6 kpc. The reduction ofthe SFR efficiency occurs earlier at higher r. While the galaxy follows theinside-out formation scenario for all r, the stars follow the inside-outscenario only up to r = 6 kpc, but for r > 6 kpc the stars follow an outside-information. The stellar formation histories inferred for each r imply that theaverage age of the stars for r > 6 increases with r.

Outside-in stellar formation in the spiral galaxy M33?