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High angular resolution spectra obtained with the Hubble Space TelescopeImaging Spectrograph (HST/STIS) provide rich morphological and kinematicalinformation about the stellar jet phenomenon, which allows us to testtheoretical models efficiently. In this work, numerical simulations of stellarjets in the propagation region are executed with the PLUTO code, by adoptinginflow conditions that arise from former numerical simulations of magnetizedoutflows, accelerated by the disk-wind mechanism in the launching region. Bymatching the two regions, information about the magneto-centrifugalaccelerating mechanism underlying a given astrophysical object can beextrapolated by comparing synthetic and observed position-velocity diagrams(PVDs). We show that quite different jets, like those from the young T Tauristars DG-Tau and RW-Aur, may originate from the same disk-wind model fordifferent configurations of the magnetic field at the disk surface. This resultsupports the idea that all the observed jets may be generated by the samemechanism.

Numerical simulations of stellar jets and comparison between synthetic and observed maps: clues to the launch mechanism