One of the puzzling questions surrounding Young Stellar Objects (YSOs) concerns the unexpected evolution of their angular momentum. Theoretically, we should expect Classical T Tauri stars (CTTs) to rotate faster due to ongoing accretion and contraction processes towards the main-sequence. Apparently, that it is not observed. Many authors suggest that the interaction star-disk has an important role towards the deceleration of these objects. Additionally, this interaction includes not only accretion, but also outflow mechanisms.

In this presentation the dynamics of accretion and outflow regions will be characterized through observations of CTTs and numerical simulations performed with PLUTO code. This study results from a collaboration between Instituto de Astrofísica e Ciências do Espaço and Observatoire de Paris.