In the D-type models we estimate the total Poynting flux by integrating over the solid angle, $S_M=\displaystyle{2\pi\int_0^{\pi}\sin\theta\overline{S(\theta )  }
   \mathrm{d} \theta}$, where $\overline{S(\theta)}$ is the mean Poynting flux in subsurface shear layer, for the range of radial distances from 0.9 to 0.99R. For the B-type models we employ the standard vacuum boundary conditions at the top of the domain.

          MEMF parts                                                                             D-type                                                                                              B-type
  --------------------------- -------------------------------------------------------------------------------------------------------------------------------------------- -----------------------------------------------------------
   $\eta_{ijk}$ -diffusivity                                                         Anisotropic, Eq.(\[eq:diff\])                                                                   Eq.(\[eq:diff\]), $C_{\delta}=0$, $a=0$
     $\alpha_{ij}$-effect                                                                 Distributed Eq.(A2)                                                                              Non-local Eq.(\[eq:babck\])
    $\gamma_{ij}$ -pumping                                                                 Eqs.(\[eq:pump\])                                                                             Eqs.(\[eq:pumpu\],\[eq:pumpb\])
        free parameters        $C_{\alpha}=0.04$,$C_{\delta}=\displaystyle{C_{\alpha}\over 3}$, $C_{\eta}=\displaystyle{1\over 15}$, $C_{v}=\displaystyle{1\over 2}$, a=3   $C_{\eta}=\displaystyle{1\over 15}$, $C_{S}=4$ ,$C_{v}=4$

Angular momentum balance
------------------------

The mean angular momentum balance in the stellar convection zone is established due to the turbulent stresses $T_{r\phi}$, $T_{\theta\phi}$, the meridional circulation and the large-scale Lorentz force [@1989drsc.book.....R] : $$\begin{aligned}
\sin\theta\frac{\partial\Omega}{\partial t} & = & \frac{1}{\rho
  r^{4}}\frac{\partial}{\partial r}r^{3}\left(T_{r\phi}
-\frac{B}{4\pi r^{2}}\frac{\partial A}{\partial\mu}\right)\label{eq:angm}\\
 & - & \frac{1}{\rho r^{2}\sin\theta}\frac{\partial}{\partial\mu}\left(\sin^{2}\theta T_{\theta\phi}-\frac{B}{4\pi r\sin\theta}\frac{\partial A}{\partial r}\right)\nonumber \end{aligned}$$ where the turbulent stresses $T_{r\phi}$ and $T_{\theta\phi}$ take into account the turbulent viscosity and generation of the large-scale shear due to the $\Lambda$- effect.

[Following to @1975JFM....67..417M, @tob1996 and @cov00, it is assumed that in the absence of the large-scale magnetic fields the solution of the Eq.(\[eq:angm\]) is time-independent and 