High Mach number convection in stellar and planetary atmospheres

High Mach number convection is a phenomenon found in stellar atmospheres. Models also predict high Mach number convection deep in the interior of gas giant planets. Our prior work in 2D domains has shown that shocks launch from convective downflow lanes at sufficiently high levels of turbulence. In this work we present simulations of fully compressible convection with parameters appropriate for gas giant planets as well as stars. We compare our models with planetary and stellar parameters to see how the dynamics of these two systems may be related. We also will present simulations that incorporate a stably stratified region above a convective region. This work is conducted using the Dedalus pseudospectral framework.