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Astrophysical jets are launched from strongly magnetized systems that host anaccretion disk surrounding a central object. The origin of the jet launchingmagnetic field is one of the open questions for modeling the accretion-ejectionprocess. Here we address the question how to generate the accretion diskmagnetization and field structure required for jet launching. Applying thePLUTO code, we present the first resistive MHD simulations of jet launchingincluding a non-scalar accretion disk mean-field $\alpha^2\Omega$-dynamo in thecontext of large scale disk-jet simulations. Essentially, we find the$\alpha_\phi$-dynamo component determining the amplification of the poloidalmagnetic field, which is strictly related to the disk magnetization (and, as aconsequence, to the jet speed, mass and collimation), while the $\alpha_R$ and$\alpha_\theta$-dynamo components trigger the formation of multiple,anti-aligned magnetic loops in the disk, with strong consequences on thestability and dynamics of the disk-jet system. In particular, such loopstrigger the formation of dynamo inefficient zones, which are characterized by aweak magnetic field, and therefore a lower value of the magnetic diffusivity.The jet mass, speed and collimation are strongly affected by the formation ofthe dynamo inefficient zones. Moreover, the $\theta$-component of the$\alpha$-dynamo plays a key role when interacting with a non-radial componentof the seed magnetic field. We also present correlations between the strengthof the disk toy dynamo coefficients and the dynamical parameters of the jetthat is launched.

MHD accretion-ejection: jets launched by a non-isotropic accretion disk dynamo. I. Validation and application of selected dynamo tensorial components