time-latitude butterfly diagrams for the toroidal field can be reproduced with (@choud95 [@dc99]) and without meridional circulation [@2011AstL...37..286K]. The distribution of the meridional circulation in the Sun is still not well established. Helioseismology measurements have deduced a double-cell structure of the meridional circulation [@Zhao13m; @2014ApJ...784..145K], while the 3D MHD simulations suggest an even more complicated structure (e.g., )

Recently, and [@2014ApJ...791...59K] discussed results of simulations for the kinematic dynamo models, which take into account the non-local $\alpha$- effect and the meridional circulation for the solar-type stars (1M$_{\odot}$) for the range of the rotational period from 1 to 30 days. These models qualitatively reproduce the increase of the magnetic activity with the increase of the rotation rate. However, the models fail to explain the decrease of the dynamo period with the increase of the rotation rate (and also the magnitude of the generated magnetic fields). found that the issue can be solved by assuming certain multiply-cell pattern of the meridional circulation.

The reverse correlation between the magnetic cycle amplitude and the cycle period is a common feature of the solar [@vetal86] and stellar [@soon94] magnetic cycles. It is fulfilled for the dynamo model with the distributed $\alpha$- effect [@pk11; @pipea2012AA]. A 