  The role of turbulent effects for dynamos in the Sun and stars continues to
be debated. Mean-field (MF) theory provides a broadly used framework to connect
these effects to fundamental magnetohydrodynamics. While inaccessible
observationally, turbulent effects can be directly studied using global
convective dynamo (GCD) simulations. We measure the turbulent effects in terms
of turbulent transport coefficients, based on the MF framework, from an
exemplary GCD simulation using the test-field method. These coefficients are
then used as an input into an MF model. We find a good agreement between the MF
and GCD solutions, which validates our theoretical approach. This agreement
requires all turbulent effects to be included, even those which have been
regarded as unimportant so far. Our results suggest that simple dynamo models,
as are commonly used in the solar and stellar community, relying on very few,
precisely fine-tuned turbulent effects, may not be representative of the full
dynamics of dynamos in global convective simulations and astronomical objects.
