Résumé
Observations and simulations have joined efforts to answer many questions raised by the unexpected behavior detected in Young Stellar Objects (YSOs). Classical T Tauri stars (CTTS) are a particular case of YSOs. These objects are interacting with their disks not only through accretion, but also through outflow processes. In this work, we will reproduce the accretion and outflow environments of RY Tau through magneto-hydrodynamical (MHD) simulations constrained by observations. Firstly, stellar activity parameters will be derived from permitted and forbidden lines in the optical spectrum of the CTTS. Secondly, we will use those parameters to adjust the simulations. In this work we reached two possible behaviors, either a steady configuration is achieved in few stellar rotations or a more turbulent one with magnetospheric ejections.