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Nonlinear saturation of solar dynamo is usually associated with the fact that mean-field dynamo action in a mirror asymmetric convection leads to a redistribution of magnetic helicity between large and small scales. Magnetic helicity accumulated in small scales suppresses so-called alpha-effect. This scenario supposes that small-scale dynamo or does not act in the Sun or the small-scale dynamo action do not contribute in the magnetic helicity redistribution. A detailed investigation of small-scale dynamo learns however a limited applicability of the above concept. In particular, small-scale dynamo action results in a magnetic helicity redistribution as well, however this process occurs in scales much smaller rather it happens for the large-scale dynamo. Here we present new data concerning nonlinear saturation of meanfield dynamo. In particular, we clarify how nonlinear saturation of small-scale dynamo occurs. The basic difference between small-scale and large-scale dynamo is that the last one contains a small parameter? Namely alpha-effect, which can be easily suppressed by the growing dynamo driven magnetic field without basic changes in other quantities responsible for dynamo action. In contrast, the only quantity which controls the small-scale dynamo is magnetic Reynolds number. Observations tell that magnetic Reynolds number remains high even at nonlinear stage of the small-scale stages of dynamo action. We demonstrate however that a suitable reorganization of hydrodynamic spectrum of magnetic convection can suppress small-scale dynamo action without basic suppression of magnetic Reynolds number.

SMALL-SCALE DYNAMO IN SPECTRAL REPRESENTATION AND NONLINEAR STABILIZATION OF SOLAR DYNAMO