2013MNRAS.429.2351R

We present and discuss results from chemical evolution models for M33. For our models we adopt a galactic formation with an inside-out scenario. The models are built to reproduce three observational constraints of the M33 disc: the radial distributions of the total baryonic mass, the gas mass, and the O/H abundance. From observations, we find that the total baryonic mass profile in M33 has a double exponential behaviour, decreasing exponentially for r ≤ 6kpc, and increasing lightly for r > 6kpc due to the increase of the gas mass surface density. To adopt a concordant set of stellar and Hii region O/H values, we had to correct the latter for the effect of temperature variations and O dust depletion. Our best model shows a good agreement with the observed radial distributions of: the star formation rate (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 formation efficiency is constant in time and space for r ≤ 6kpc, but the SFR efficiency decreases with time and galactocentric distance for r > 6kpc. The reduction of the SFR efficiency occurs earlier at higher r. While the galaxy follows the inside-out formation scenario for all r, the stars follow the inside-out scenario only up to r = 6kpc, but for r > 6kpc the stars follow an outside-in formation. The stellar formation histories inferred for each r imply that the average age of the stars for r > 6 increases with r.