Abstract

The structural parameters of the Large Magellanic Cloud and the Small Magellanic Cloud are derived from the study of dierent stellar populations, such as, Cepheids (age ~ 100 Myr), Red Clump stars (age ~ 2-9 Gyr) and RR Lyrae stars (age ~ > 9 Gyr). The structural changes of these galaxies as a function of time are identified and the processes which are responsible for these changes are discussed. The formation and early evolution of these two galaxies are found to be different.