Rotating convection is a fundamental process that underlies many phenomena in geophysics and astrophysics. Besides theory and experiments, numerical simulations are crucial tools in these fields. Here, I will review the most commonly used idealised simulation geometries and discuss their respective advantages and drawbacks, with a particular focus on cylindrical geometries. I will also highlight the significance of the Prandtl number in rotating convection. This control parameter is arguably the hardest to vary in experiments, thus, I will showcase one of the great advantages of numerical over experimental approaches. Finally, I will briefly address simulations of rotating magnetoconvection, emphasising the importance of understanding the interplay of the Coriolis and the Lorentz force in geophysical and astrophysical fluid dynamics.
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