Compositional Turbulence and Layering in the Gaseous Envelopes of Forming Planets

TL;DR

This paper investigates how dust grain growth and settling in forming planetary envelopes can induce compositional turbulence via thermohaline instability, affecting planetary structure and potentially leaving observable signatures.

Contribution

It reveals that dust-driven compositional turbulence occurs in planetary envelopes, especially at super-AU distances, and explores implications for planetary formation and layering.

Findings

Compositional turbulence driven by thermohaline instability occurs in planetary envelopes.

Turbulence is more effective at super-AU distances than at sub-AU.

Different turbulent regimes may influence the final planetary structure.

Abstract

Differential settling and growth of dust grains impact the structure of the radiative envelopes of gaseous planets during formation. Sufficiently rapid dust growth can result in envelopes with substantially reduced opacities for radiation transport, thereby facilitating planet formation. We revisit the problem and establish that dust settling and grain growth also lead to outer planetary envelopes that are prone to compositional instabilities, by virtue of their inverted mean-molecular weight gradients. Under a variety of conditions, we find that the radiative envelopes of forming planets experience compositional turbulence driven by a semi-transparent version of the thermohaline instability ('fingering convection'). The compositional turbulence seems efficient at mixing dust in the radiative envelopes of planets forming at super-AU distances (say $5$ AU) from a Sun-like star, but not so at sub-AU distances (say $0.2$ AU). We also address the possibility of compositional layering in this context. Distinct turbulent regimes for planetary envelopes growing at sub-AU vs. super-AU distances could leave an imprint on the final planets formed.