To cool is to keep: Residual H/He atmospheres of super-Earths and sub-Neptunes

TL;DR

This paper demonstrates that some super-Earths can retain small residual hydrogen/helium atmospheres after core-powered mass-loss, affecting their evolution and observable properties.

Contribution

It introduces a model showing residual H/He envelope retention is possible, depending on planet mass and temperature, and explores its implications for planetary evolution.

Findings

Residual H/He envelopes can be retained, ranging from <10^-8 to 10^-3 of planet mass.

Retention depends on planet mass, temperature, initial envelope, and opacity.

Residual atmospheres influence long-term planetary evolution and observability.

Abstract

Super-Earths and sub-Neptunes are commonly thought to have accreted hydrogen/helium envelopes, consisting of a few to ten percent of their total mass, from the primordial gas disk. Subsequently, hydrodynamic escape driven by core-powered mass-loss and/or photo-evaporation likely stripped much of these primordial envelopes from the lower-mass and closer-in planets to form the super-Earth population. In this work we show that after undergoing core-powered mass-loss, some super-Earths can retain small residual H/He envelopes. This retention is possible because, for significantly depleted atmospheres, the density at the radiative-convective boundary drops sufficiently such that thhe cooling time-scale becomes less than the mass-loss time-scale. The residual envelope is therefore able to contract, terminating further mass loss. Using analytic calculations and numerical simulations, we show that the mass of primordial H/He envelope retained as a fraction of the planet's total mass, $f_{ret}$, increases with increasing planet mass, $M_{c}$, and decreases with increasing equilibrium temperature, $T_{eq}$, scaling as $f_{ret} \propto M_{c}^{3/2} T_{eq}^{-1/2} \exp{[M_{c}^{3/4} T_{eq}^{-1}]}$. $f_{ret}$ varies from $< 10^{-8}$ to about $10^{-3}$ for typical super-Earth parameters. To first order, the exact amount of left-over H/He depends on the initial envelope mass, the planet mass, its equilibrium temperature, and the envelope's opacity. These residual hydrogen envelopes reduce the atmosphere's mean molecular weight compared to a purely secondary atmosphere, a signature observable by current and future facilities. These remnant atmospheres may, however, in many cases be vulnerable to long-term erosion by photo-evaporation. Any residual hydrogen envelope likely plays an important role in the long-term physical evolution of super-Earths, including their geology and geochemistry.