New stars are formed by the collapse of cold, dense molecular cloud cores. Between 10 thousand and 10 million years after the onset of collapse, the protostar is initially revealed, and its protoplanetary disk is eventually dissipated.

In this talk, I will present our efforts to model observations of these systems and investigate how they change as a function of evolutionary state. Finally, I will discuss possible observational signatures of planet formation in the protoplanetary disk.