  We present a method to characterize the spectral transfers of magnetic energy
between scales in simulations of stellar convective dynamos. The full triadic
transfer functions are computed thanks to analytical coupling relations of
spherical harmonics based on the Clebsch-Gordan coefficients. The method is
applied to mean field $\alpha\Omega$ dynamo models as benchmark tests. From the
physical standpoint, the decomposition of the dynamo field into primary and
secondary dynamo families proves very instructive in the $\alpha\Omega$ case.
The same method is then applied to a fully turbulent dynamo in a solar
convection zone, modeled with the 3D MHD ASH code. The initial growth of the
magnetic energy spectrum is shown to be non-local. It mainly reproduces the
kinetic energy spectrum of convection at intermediate scales. During the
saturation phase, two kinds of direct magnetic energy cascades are observed in
regions encompassing the smallest scales involved in the simulation. The first
cascade is obtained through the shearing of magnetic field by the large scale
differential rotation that effectively cascades magnetic energy. The second is
a generalized cascade that involves a range of local magnetic and velocity
scales. Non-local transfers appear to be significant, such that the net
transfers cannot be reduced to the dynamics of a small set of modes. The
saturation of the large scale axisymmetric dipole and quadrupole are detailed.
In particular, the dipole is saturated by a non-local interaction involving the
most energetic scale of the magnetic energy spectrum, which points out the
importance of the magnetic Prandtl number for large-scale dynamos.
