  The 3D thermal convection in the Boussinesq approximation with heating from
below and dynamo in the cube are considered. We study dependence of the
convection intensity and magnetic field generation on the latitude in
$\beta$-plane approximation. It is shown that kinetic energy gradually
increases from the poles to the equator more than order of magnitude. The model
predicts the strong azimuthal thermal wind, which direction depends on the sign
of the thermal convective fluctuations. The spatial scale of the arising flow
is comparable to the scale of the physical domain. The magnetic energy
increases as well, however dynamo efficiency, i.e., the ratio of the magnetic
energy to the kinetic one decreases to the equator. This effect can explain
predominance of the dipole configuration of the magnetic field observed in the
planets and stars. The approach is useful for modeling of the
magnetohydrodynamic turbulence in planetary cores and stellar convective zones.
