  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.
