Star-in-a-box simulations of fully convective stars

(abridged) Context: Main-sequence late-type stars with masses less than $0.35 M_\odot$ are fully convective. Aims: The goal is to study convection, differential rotation, and dynamos as functions of rotation in convective stars. Methods: Three-dimensional hydrodynamic magnetohydrodynamic numerical simulations a star-in-a-box model, where spherical star immersed inside Cartesian cube, used. model corresponds $0.2M_\odot$ M5 dwarf. Rotation periods ($P_{\rm rot}$) between 4.3 430 days explored. Results: slowly rotating $P_{\rm rot}=430$ produces anti-solar slow equator fast poles, along predominantly axisymmetric quasi-steady large-scale magnetic fields. For intermediate rot}=144$ $43$ days) solar-like (fast equator, poles) fields mostly either quasi-stationary or cyclic. latter occurs similar parameter regime other studies shells, the cycle period observed cycles comparable rot}$. In rapid weak increasingly non-axisymmetric dominating $m=1$ mode. This field also exhibits azimuthal dynamo waves. Conclusions: results models agree partially shells that transitions regimes occur at rotational terms Coriolis (inverse Rossby) number. similarity suggests processes generating magnetism insensitive geometry star.