Description
This talk will summarize the state of affairs on what's often called the "Convective conundrum." While ostensibly not having much to do with rotation, it's actually all about what we know regarding the degree of influence rotation has on interior flow amplitudes and the overall dynamical scales. The conundrum part comes from not seeing giant-scale motions at the surface. Is this null result because of poor signal-to-noise? Or are the long-default convective structure truly absent?
The talk will discuss some of the possible physics of rapidly rotating convection as well as how supergranulation might be conducting a coverup. I'll make the case that theory and simulations give good guesses about what's happening. But a definitive solution will likely have to wait for more and better data, hopefully coming from the polar regions where convection most feels that Coriolis effect.
