The energy for driving turbulent flows in planetary fluid layers comes from a combination of thermocompositional sources and the motion of the boundary in contact with the fluid through mechanisms like precessional, tidal, and librational forcing. Characterizing the resulting turbulent fluid motions are necessary for understanding a planet’s dynamics and evolution including the generation of magnetic fields in the electrically conducting fluid layers and dissipation in the oceans. I will describe two unique sets of laboratory experiments that replicate the fundamental ingredients of thermal convection and mechanical forcing and show analysis of this turbulent flow using thermometry and velocimetry data. These new results challenge the findings of present day models of fluid motions in planetary interiors.