The spatial and temporal evolution of corotating interaction regions is examined between 0.5 and 30 AU using a solar wind simulation with a continuous sinusoidally varying velocity, density, and temperature input pulse train. We show (1) the well-known formation of forward-reverse MHD shock ensembles, followed by (2) their interaction that results in a highly nonlinear ''pressure'' wave that eventually reforms into a new but more irregular set of forward-reverse shock pairs. As a result of these compound interactions, the overall temperature decays much more slowly than the classical steady state adiabatic radial dependency of R-4/3.