  We have constructed the foundations to a series of theoretical diagnostic
methods to probe the jet phenomenon in young stars as observed at various
optical forbidden lines. We calculate and model in a self-consistent manner the
physical and radiative processes which arise within an inner disk-wind driven
magnetocentrifugally from the circumstellar accretion disk of a young sun-like
star. Comparing with real data taken at high angular resolution, our approach
will provide the basis of systematic diagnostics for jets and their related
young stellar objects, to attest the emission mechanisms of such phenomena.
This work can help bring first-principle theoretical predictions to confront
actual multi-wavelength observations, and will bridge the link between many
very sophiscated numerical simulations and observational data. Analysis methods
discussed here are immediately applicable to new high-resolution data obtained
with HST and Adaptic Optics.
