Astrophysical jets are launched from strongly magnetized systems that host an accretion disk surrounding a central object. Applying the PLUTO code, we present the first resistive MHD simulations of jet launching, including a non-scalar accretion-disk mean-field dynamo in the context of large-scale disk-jet simulations. We disentangled the effects of the dynamo components, showing how the amplification of the magnetic field and the formation of magnetic loops are connected with the mean-field dynamo. We have also investigated how the initial magnetic field seed affects the large-scale structure and evolution, confirming that the mean-field dynamo in accretion disks is non-isotropic. We have then investigated a disk dynamo that follows analytical solutions of the mean-field dynamo theory, essentially based only on a single parameter, the Coriolis number. We have also presented correlations between the strength of the disk dynamo coefficients and the dynamical parameters of the jet that is launched, and discussed their implications for observed jet quantities.
By carrying out nonideal MHD simulations (PLUTO code), we investigated how the feedback of the generated magnetic field on the mean-field dynamo affects the disk and jet properties. We found that a stronger quenching of the dynamo leads to a saturation of the magnetic field at a lower disk magnetization. Nevertheless, we found that, while applying different dynamo feedback models, the overall jet properties remained unaffected. We then investigated a feedback model that encompasses a quenching of the magnetic diffusivity. Our modeling considers a more consistent approach for mean-field dynamo modeling simulations, as the magnetic quenching of turbulence should be considered for both a turbulent dynamo and turbulent magnetic diffusivity. We found that, after the magnetic field is saturated, the Blandford–Payne mechanism can work efficiently, leading to more collimated jets, which move, however, at a slower speed. We found strong intermittent periods of flaring and knot ejection for low Coriolis numbers. In particular, flux ropes are built up and advected toward the inner disk, thereby cutting off the inner disk wind, leading to magnetic field reversals, reconnection, and the emergence of intermittent flares.