Supernova (SN) light curves can be powered by two different energy sources: internal energy that was deposited by the shock wave during the explosion, and radioactive emission from decaying unstable isotopes. The interplay between their contributions, together with different progenitor properties, creates a diversity in the observed SN light curves. Analytic modeling can thus help unveil the dependence of the light curve shape on progenitor properties, and explain the variety seen in observations. In this talk I will discuss two works - in the first one, we use self similar solutions to model the early SN light curves and find a correction to the dynamics of the SN during the early planar phase. In the second project, we model the subsequent hydrogen recombination phase, and explain the formation of the `plateau' - a phase of almost constant luminosity, that characterizes type II-P SN light curves.