Axisymmetric simulations of the convective overstability in protoplanetary discs

TL;DR

This study uses axisymmetric simulations to explore the convective overstability in protoplanetary discs, revealing how it evolves through different saturation regimes and impacts planet formation processes.

Contribution

First detailed simulation analysis of convective overstability saturation routes in protoplanetary discs, highlighting the transition from wave turbulence to zonal flows.

Findings

Parasites halt exponential growth of COS

Transition from wave turbulence to zonal flows with increasing Reynolds number

Zonal flows likely spawn vortices affecting planet formation

Abstract

Protoplanetary discs at certain radii exhibit adverse radial entropy gradients that can drive oscillatory convection (`convective overstability'; COS). The ensuing hydrodynamical activity may reshape the radial thermal structure of the disc while mixing solid material radially and vertically or, alternatively, concentrating it in vortical structures. We perform local axisymmetric simulations of the COS using the code SNOOPY, showing first how parasites halt the instability's exponential growth, and second, the different saturation routes it takes subsequently. As the Reynolds and (pseudo-) Richardson numbers increase, the system moves successively from (a) a weakly nonlinear state characterised by relatively ordered nonlinear waves, to (b) wave turbulence, and finally to (c) the formation of intermittent and then persistent zonal flows. In three-dimensions, we expect the latter flows to spawn vortices in the orbital plane. Given the very high Reynolds numbers in protoplanetary discs, the third regime should be the most prevalent. As a consequence, we argue that the COS is an important dynamical process in planet formation, especially near features such as dead zone edges, ice lines, gaps, and dust rings.