  In this work, we have studied the variability and frequency of occurrence of
the grand minima using kinematic dynamo models of one solar mass star with
different rotation rates and depths of convection zones. We specify the
large-scale flows (differential rotations and meridional circulations) from
corresponding hydrodynamic models. We include stochastic fluctuations in the
Babcock-Leighton source for the poloidal field to produce variable stellar
cycles. We observe that the rapidly rotating stars produce highly irregular
cycles with strong magnetic fields and rarely produce Maunder-like grand
minima, whereas the slowly rotating stars (Sun and longer rotation period)
produce smooth cycles of weaker strength and occasional grand minima. In
general, the number of the grand minima increases with the decrease in rotation
rate. These results can be explained by the fact that with the increase of
rotation period, the supercriticality of the dynamo decreases, and the dynamo
is more prone to produce extended grand minima in this regime.
