  Theoretical Period-Age and Period-Age-Color relations for different chemical
compositions have been recently derived using an updated homogeneous set of
evolutionary and pulsational models. We apply these relations to Cepheids in
the Magellanic Clouds to constrain the recent star formation history of these
dwarf galaxies. Finally, we also compare the radial distribution of classical
Cepheids with young clusters and star forming regions.
