  Astrophysical jets are launched from strongly magnetized systems that host an
accretion disk surrounding a central object. Here we address the question how
to generate the accretion disk magnetization and field structure required for
jet launching. We continue our work from Paper I (Mattia & Fendt 2020a),
considering a non-scalar accretion disk mean-field $\alpha^2\Omega$-dynamo in
the context of large scale disk-jet simulations. We now investigate a disk
dynamo that follows analytical solutions of mean-field dynamo theory,
essentially based only on a single parameter, the Coriolis number. We thereby
confirm the anisotropy of the dynamo tensor acting in accretion disks, allowing
to relate both the resistivity and mean-field dynamo to the disk turbulence.
Our new model recovers previous simulations applying a purely radial initial
field, while allowing for a more stable evolution for seed fields with a
vertical component. We also present correlations between the strength of the
disk dynamo coefficients and the dynamical parameters of the jet that is
launched, and discuss their implication for observed jet quantities.
