the general stellar parameters, such as mass, age , the spectral class and the rotation rate. The mass of a star and its Rossby number, which is the ratio of the period of rotation and a typical turnover time of convection, are likely the most important parameters governing the stellar dynamo [@2009ARAA_donat; @2013AN....334...48M]. The diagram 3 in the paper by @2009ARAA_donat shows an increase of the magnetic activity with decrease of the Rossby number and the mass of a star. These parameters determine the topology of the large-scale magnetic field, as well. It is found that the axisymmetric solar-type dynamo can operates in stars with mass about $1M_{\odot}$, and with periods of rotation longer than 10 days. [Observations, also show evidences that solar analogs with period of rotation smaller than 10 days, may have]{} the substantial non-axisymmetric components of the large-scale magnetic field [@2009ARAA_donat; @2014IAUS..302..110F].

Interpretation of the stellar magnetic activity is rather complicated because of nonlinear dynamo effects that needs to be taken into account [@soon93; @1999ApJ_sa_br; @2007ApJ_bohm; @2011IAUS_saar; @2015MNRAS.446L..51B]. Moreover, even for the solar dynamo processes many details are poorly known. [@chrev05]. In particular, the origin of the large-scale poloidal magnetic field of the Sun (the component of 