tokens: of the α-effect and the angular velocity profile, the star with the rotation period of 30 d is slightly above the large-scale dynamo instability threshold. Table 1 lists the integral parameters for the kinematic dynamo models. Our results are in general agreement with the results of the previous paper by Pipin ( 2015 ). The models show a decrease in the dynamo period with an increase in the rotation rate. Fig. 3 shows the time–latitude diagrams for the large-scale toroidal magnetic field evolution at r = 0.9 R in the kinematic models. The models with a period of rotation longer than 10 d show solar-like butterfly diagrams. The star rotating with a period of 10 d shows a double dynamo wave pattern, where the high-frequency high-latitude cycles merge into long cycles at low latitudes. A similar pattern is found for the star rotating with the period of 8 d. For a star with a higher rotation rate, the dynamo wave patterns divide into two: the high-latitude wave drifts to the equator and the low-latitude wave migrates toward the poles. This property becomes very clear for the M5, M2 and M1 models. All these models show a mix of the magnetic parity modes and different systems of the dynamo waves at high and low latitudes. The complicated dynamo wave patterns in these models result in multiple dynamo periods (see Table 1 ). For example, the model M1 shows three different dynamo waves. There are two high-frequency waves migrating toward the poles below 50°. The third wave is a quasi-periodic high-latitude wave migrating toward the equator. We deduce the dynamo periods using the time–latitude diagrams of the toroidal magnetic field in the subsurface layer r = 0.9 R , the variations of the toroidal magnetic field flux F S , and the Poynting flux luminosity L P . To identify the dynamo periods, we employ the standard wavelet package of the scipy distribution (see www.scipy.org ). All these parameters indicate the unique dynamo period for the models in the range of rotational periods from 15 to 30 d. The models for a rotational period of less than 15 d start to show long-term variations. The different dynamo parameters show the different sets of periodic variations. For the long period, we choose the minimal value that is found both in F S and L P and in the time–latitude diagrams. Also, the models for fast rotating stars, M1, M2 and M5, show the short-term periodicity of the L P parameter. Its period is about two times less than the main dynamo period. Figure 3. The time–latitude diagrams for the near-surface ( r = 0.9 R ) toroidal magnetic fields for the kinematic dynamo models. Table 1. The integral parameters of the kinematic dynamo models. The numbers in the model names correspond to the period of rotation in days, which is rounded to the nearest integer. P rot is the period of stellar rotation. Ro* is the estimation of the Rossby number. F T is the magnitude of the total magnetic flux in the convection zone. F S is the magnitude of the
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