Many objects studied in the context of stellar and extragalactic astronomy fall into the category of accretion ejection systems, such as young stars and radio loud active galactic nuclei. Since these systems are far from transient in their timescales, the issue of temporal stability can be efficiently addressed through high resolution MHD numerical simulations of resistive magnetized accretion disks launching a supersonic jet, in a self-consistent way. To this perspective, we present a series of simulations performed using the PLUTO code that aim to study the parameters of such systems and discuss how these affect their properties (eg. ejection efficiency, transfer of energy and angular momentum, magnetic field topology and collimation) and their capability to reach a quasi-stationary final state.