We review some of the models of chemical evolution of ellipticals and bulges of spirals .
In particular , we focuse on the star formationn histories of ellipticals and their influence on chemical properties such as the [ \alpha /Fe ] versus [ Fe/H ] , galactic mass and visual magnitudes .
By comparing models with observational properties , we can constrain the timescales for the formation of these galaxies .
The observational properties of stellar populations suggest that the more massive ellipticals formed on a shorter timescale than less massive ones , in the sense that both the star formation rate and the mass assembly rate , strictly linked properties , were more efficient in the most massive objects .
Observational properties of true bulges seem to suggest that they are very similar to ellipticals and that they formed on a very short timescale : for the bulge of the Milky Way we suggest a timescale of 0.1 Gyr .
This leads us to conclude that the Bulge evolved in a quite independent way from the galactic Disk .