  We investigate dynamo action in global compressible solar-like convective
dynamos in the framework of mean-field theory. We simulate a solar-type star in
a wedge-shaped spherical shell, where the interplay between convection and
rotation self-consistently drives a large-scale dynamo. To analyze the dynamo
mechanism we apply the test-field method for azimuthally ($\phi$) averaged
fields to determine the 27 turbulent transport coefficients of the
electromotive force, of which six are related to the $\alpha$ tensor. This
method has previously been used either in simulations in Cartesian coordinates
or in the geodynamo context and is applied here for the first time to fully
compressible simulations of solar-like dynamos. We find that the
$\phi\phi$-component of the $\alpha$ tensor does not follow the profile
expected from that of kinetic helicity. The turbulent pumping velocities
significantly alter the effective mean flows acting on the magnetic field and
therefore challenge the flux transport dynamo concept. All coefficients are
significantly affected by dynamically important magnetic fields. Quenching as
well as enhancement are being observed. This leads to a modulation of the
coefficients with the activity cycle. The temporal variations are found to be
comparable to the time-averaged values and seem to be responsible for a
nonlinear feedback on the magnetic field generation. Furthermore, we quantify
the validity of the Parker-Yoshimura rule for the equatorward propagation of
the mean magnetic field in the present case.
