confirmed by @vid14MNR who found $\delta\approx1.61$ for the X-ray flux for magnetic activity in solar type stars. The flux reaches the magnitude $10^{-3}F_{\odot}$, where $F_{\odot}={\displaystyle \frac{L_{\odot}}{4\pi R_{\odot}^{2}}}$. The result is in the agreement with the observational findings [@2006ARep_kazova]. We postpone the detailed study of the Poynting flux in the nonlinear dynamo for the future.

[In our calculations we compute the averaged surface magnetic field, as well. The results for this proxy of the stellar magnetic activity were published recently by [@vid14MNR]. For the given range of the rotation rates both the D- and B-types of the dynamo models reproduce the observational finding reasonably well. We postpone a more detailed comparison of these results with observations for a future.]{}

[It is noteworthy that the feedback of the magnetic helicity quenching on the large-scale dynamo depends on amount of the magnetic helicity in the dynamo region. This is partly controlled by the effective magnetic Reynolds number, $R_m$. The decrease of the $R_m$ simulates the increase of the helicity loss. It is found that for the $R_m=10^2$ the model D3 produces nearly the same amount of the total magnetic flux as the model D2. The similar effect can be expected for the B-type 