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Simulations of magnetohydrodynamics convection in slowly rotating starspredict anti-solar differential rotation (DR) in which the equator rotatesslower than poles. This anti-solar DR in the usual $\alpha \Omega$ dynamo modeldoes not produce polarity reversal. Thus, the features of large-scale magneticfields in slowly rotating stars are expected to be different than stars havingsolar-like DR. In this study, we perform mean-field kinematic dynamo modellingof different stars at different rotation periods. We consider anti-solar DR forthe stars having rotation period larger than 30~days and solar-like DRotherwise. We show that with particular $\alpha$ profiles, the dynamo modelproduces magnetic cycles with polarity reversals even with the anti-solar DRprovided, the DR is quenched when the toroidal field grows considerably highand there is a sufficiently strong $\alpha$ for the generation of toroidalfield. Due to the anti-solar DR, the model produces an abrupt increase ofmagnetic field exactly when the DR profile is changed from solar-like toanti-solar. This enhancement of magnetic field is in good agreement with thestellar observational data as well as some global convection simulations. Inthe solar-like DR branch, with the decreasing rotation period, we find themagnetic field strength increases while the cycle period shortens. Both ofthese trends are in general agreement with observations. Our study providesadditional support for the possible existence of anti-solar DR in slowlyrotating stars and the presence of unusually enhanced magnetic fields andpossibly cycles which are prone to production of superflare.

Stellar Dynamos with Solar and Anti-solar Differential Rotations: Implications to Magnetic Cycles of Slowly Rotating Stars