The physical mechanisms involved in the evolution of Young Stellar Objects (YSOs) are a complex subject still under debate. Classical T Tauri stars (CTTS) are solar-like stars that are not only accreting mass from their circumstellar disks, but are also ejecting part of it in different shapes of outflows. At the moment, the star-disk interaction seems to be responsible for the angular momentum extraction. Besides being held by strong magnetic fields, it includes also accretion and outflow processes. The aim of this study is to characterize the dynamics of accretion and outflow regions under both observations and magnetohydrodynamic (MHD) numerical simulations of CTTS.