Outflows and jets are an integral part of the formation of young stars and are found to be commonplace in all regions where star formation is known to occur. There has been much work done in the development of computational fluid dynamic methods for the simulation of these outflows in an attempt to gam a greater insight into the processes taking place in their formation. Observational data presents key characteristics of such outflows that can be used to determine the validity of any computational model. Here, we have developed a sophisticated parallehsation method for the splittingup of a jet simulation across a Beowulf type computer cluster using a message-passing method. The parallelised code allows us to run simulations for much longer and on larger domains than was possible with the original serial code. This allows us to investigate the development of some important characteristics of the computational model over large time-scales with a suitably high resolution. In particular we investigate the behaviour of the mass-velocity and mtensity-velocity relationships for molecular outflows driven by a prompt-entramment type jet model. Up to now simulations have indicated good agreement between these characteristics for this model and the observed behaviour of these relationships. However, the short time-scales used did not allow for an evolutionary study of the relationships and as a result long-term simulations are deemed necessary.