We present results from a three‐dimensional model of the Saturnian radiation belts. This model draws on pre‐existing physical radiation‐belt models, developed to study the belts of the Earth and Jupiter. In the present work, transport processes and interactions with dust and gas clouds, moons, and plasma are considered to determine the trapped particle distribution in Saturn's inner magnetosphere. The results of the modeling are: absorption by dust is the dominant loss effect in the innermost region while local losses from satellites act as the prominent physical process in the outer part of the inner magnetosphere. Results suggest strong energetic neutral atom emission and weak synchrotron emission. Comparisons between data and model results are presented.