  High angular resolution spectra obtained with the Hubble Space Telescope
Imaging Spectrograph (HST/STIS) provide rich morphological and kinematical
information about the stellar jet phenomenon, which allows us to test
theoretical models efficiently. In this work, numerical simulations of stellar
jets in the propagation region are executed with the PLUTO code, by adopting
inflow conditions that arise from former numerical simulations of magnetized
outflows, accelerated by the disk-wind mechanism in the launching region. By
matching the two regions, information about the magneto-centrifugal
accelerating mechanism underlying a given astrophysical object can be
extrapolated by comparing synthetic and observed position-velocity diagrams
(PVDs). We show that quite different jets, like those from the young T Tauri
stars DG-Tau and RW-Aur, may originate from the same disk-wind model for
different configurations of the magnetic field at the disk surface. This result
supports the idea that all the observed jets may be generated by the same
mechanism.
