  We present multi-dimensional simulations of magnetized radiative jets
appropriate to Young Stellar Objects. Magnetized jets subject to collisionally
excited radiative losses have not, as yet, received extensive scrutiny. The
purpose of this letter is to articulate the propagation dynamics of radiative
MHD jets in the context of the extensive jet literature. Most importantly, we
look for morphological and kinematic diagnostics that may distinguish
hydrodynamic protostellar jets from their magnetically dominated cousins. Our
simulations are axisymmetric (2.5-D). A toroidal B_phi field geometry is used.
Our models have high sonic Mach numbers (Ms approx 10), but lower fast mode
Mach number (Mf approx 5). This is approximately the case for jets formed via
disk-wind or X-wind models - currently the consensus choice for launching and
collimating YSO jets. Time-dependent radiative losses are included via a
coronal cooling curve. Our results demonstrate that the morphology and
propagation characteristics of strongly magnetized radiative jets can differ
significantly from jets with weak fields. In particular the formation of
nose-cones via post-shock hoop stresses leads to narrow bow shocks and enhanced
bow shock speeds. In addition, the hoop stresses produce strong shocks in the
jet beam which constrasts with the relatively unperturbed beam in radiative
hydrodynamic jets. Our simulations show that pinch modes produced by magnetic
tension can strongly effect magnetized protostellar jets.
