We present preliminary results from a new chemical evolution model meant to be a first step in the self-consistent study of both optical and X-ray properties of elliptical galaxies in cluster of galaxies. Detailed cooling and heating processes in the interstellar medium are taken into account using a mono-phase one-zone treatment which allows a more reliable modelling of the galactic wind regime with respect to previous work. The model successfully reproduces simultaneously the mass-metallicity, colour-magnitude, the LX LB and the LX T relations, as well as the ob- ratio as a function of σ, by assuming that the gas infall and star served trend of the  formation timescales are shorter for brighter objects. We found that a late secondary accretion of gas from the environment might play a role in driving the LX LB and LX T relations and can explain their large observational scatter. The iron discrepancy, namely the too high predicted iron abundance in X-ray haloes of ellipticals compared to observations, still persists. On the other hand, we predict [O/Fe] in the ISM which is in good agreement with the most recent observations. New predictions for the amounts of iron, oxygen and energy ejected into the intracluster medium are presented and we conclude that Type Ia supernovae play a fundamental role in the ICM enrichment. SNe Ia activity, in fact, may power a galactic wind lasting for a considerable amount of the galactic lifetime, even in the case for which the efficiency of energy transfer into the ISM per SN Ia event is less than unity.