  It has been recently shown that a small-scale dynamo (SSD) instability could
be possible in solar-like low magnetic Prandtl number Pm plasmas. It has been
proposed that the presence of SSD can potentially have a significant impact on
the dynamics of the large-scale dynamo (LSD) in the stellar convection zones.
Studying these two dynamos, SSD and LSD, together in a global magnetoconvection
model requires high-resolution simulations and large amounts of computational
resources. Starting from a well-studied global convective dynamo model that
produces cyclic magnetic fields, we systematically increased the resolution and
lowered the diffusivities to enter the regime of Reynolds numbers that allow
for the excitation of SSD on top of the LSD. We studied how the properties of
convection, generated differential rotation profiles, and LSD solutions change
with the presence of SSD. We performed convective dynamo simulations in a
spherical wedge with the Pencil Code. The resolutions of the models were
increased in 4 steps by a total factor of 16 to achieve maximal fluid and
magnetic Reynolds numbers of over 500. We found that the differential rotation
is strongly quenched by the presence of the LSD and SSD. Even though the
small-scale magnetic field only mildly decreases increasing Re, the large-scale
field strength decreases significantly. We do not find the SSD dynamo
significantly quenching the convective flows as claimed recently by other
authors; in contrast, the convective flows first grow and then saturate for
increasing Re. Furthermore, the angular momentum transport is highly affected
by the presence of small-scale magnetic fields, which are mostly generated by
LSD. These fields not only change the Reynolds stresses, but also generate
dynamically important Maxwell stresses. The LSD evolution in terms of its
pattern and field distribution is rather independent of the increase in Rm.
