RELAXATION TIME AND DISSIPATION INTERACTION IN HOT PLANET ATMOSPHERIC FLOW SIMULATIONS

We elucidate the interplay between Newtonian thermal relaxation and numerical dissipation, of several different origins, in flow simulations of hot extrasolar planet atmospheres. Currently, a large range of Newtonian relaxation, or "cooling," times (similar to 10 days to similar to 1 hr) is used among different models and within a single model over the model domain. In this study, we demonstrate that a short relaxation time (much less than the planetary rotation time) leads to a large amount of unphysical, grid-scale oscillations that contaminate the flow field. These oscillations force the use of an excessive amount of artificial viscosity to quench them and prevent the simulation from " blowing up." Even if the blow-up is prevented, such simulations can be highly inaccurate because they are either severely overdissipated or underdissipated, and are best discarded in these cases. Other numerical stability and time step size enhancers (e.g., Robert-Asselin filter or semi-implicit time-marching schemes) also produce similar, but less excessive, damping. We present diagnostics procedures to choose the "optimal" simulation and discuss implications of our findings for modeling hot extrasolar planet atmospheres.