Numerical simulations of magnetohydrodynamics (MHD) have led to reasonable descriptions of the general morphology and dynamics of Earth's magnetosphere. However, MHD is invalid in regions close to the Earth where gradient and curvature drifts are comparable to the E × B drift. The Rice Convection Model was designed to take into account such dynamics and provide a more realistic description of the plasma distribution, using an input magnetic field model such as the Lyon Fedder Mobarry (LFM). Recent efforts to couple the RCM and the LFM have led to a more complete picture of magnetospheric processes. This thesis describes the physics of the two regions, our coupling paradigm, and analysis tools for interpreting these results.