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 { 1 \over 2 } -D ) .
A toroidal ( B _ { \phi } ) field geometry is used .
Our models have high sonic Mach numbers ( M _ { s } \approx 10 ) , but lower fast mode Mach number ( M _ { f } \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 .
These differences may be useful in observational studies designed to distinguish between competing jet collimation scenarios .