| Sumario: | In the majority of models, the protoplanetary disks have a continuous distribution of gas and dust, with a dynamics that gives origin to the planets, which in the process of formation, make grooves on the disk by gravitationally capturing the existing matter around them. Transition disks are a class of protoplanetary disk that has a large cavity free of gas and dust inside. In this paper a statistical model based on transitional discs is proposed, which extends to protoplanetary disks. With this model you can perform dynamic simulations of planetary formation using few parameters. The process followed to simulate the transition disk DoAr44 and the protoplanetary disk Hl-Tauri is shown. Unlike other models, the formation of planetary bodies is faster.
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