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In stars and planets natural processes heat convective flows in the bulk of aconvective region rather than at hard boundaries. By characterizing howconvective dynamics are determined by the strength of an internal heatingsource we can gain insight into the processes driving astrophysical convection.Internally heated convection has been studied extensively in incompressiblefluids, but the effects of stratification and compressibility have not beenexamined in detail. In this work, we study fully compressible convection drivenby a spatially uniform heating source in 2D and 3D Cartesian, hydrodynamicsimulations. We use a fixed temperature upper boundary condition which resultsin a system that is internally heated in the bulk and cooled at the top. Wefind that the flow speed, as measured by the Mach number, and turbulence, asmeasured by the Reynolds number, can be independently controlled by separatelyvarying the characteristic temperature gradient from internal heating and thediffusivities. 2D simulations at a fixed Mach number (flow speed) demonstrateconsistent power at low wavenumber as diffusivities are decreased. We observeconvection where the velocity distribution is skewed towards cold, fastdownflows, and that the flow speed is related to the length scale and entropygradient of the upper boundary where the downflows are driven. We additionallyfind a heat transport scaling law which is consistent with prior incompressiblework.

Internally heated and fully compressible convection: flow morphology and scaling laws