Abstract
Classical T Tauri stars (CTTS) are known to be magnetically active pre-main sequence stars showing evidences of circumstellar accretion disks. Despite the fact that they are still actively contracting and accreting, they are characterized by long and constant periods of rotation. In this work I present numerical magnetohydrodynamic (MHD) simulations of the interaction between a viscous and resistive accretion disk with a dipolar stellar magnetosphere. The aim of these simulations is to illustrate different mechanisms which can contribute in controlling the period of rotation of the protostar.
