Atmosphere loss in planet-planet collisions

TL;DR

This study uses SPH simulations to investigate how giant planet collisions can strip atmospheres, revealing two regimes of mass loss and providing scaling laws for atmosphere retention based on impact energy.

Contribution

It introduces a detailed analysis of atmosphere loss regimes in planetary collisions and offers scalable algorithms for future modeling efforts.

Findings

Atmosphere loss occurs in two regimes: outer layer ejection and core/mantle excavation.

Approximately 20% atmosphere remains at the transition energy between regimes.

Atmosphere loss scales quadratically with the ratio of impact energy to transition energy.

Abstract

Many of the planets discovered by the Kepler satellite are close orbiting Super-Earths or Mini-Neptunes. Such objects exhibit a wide spread of densities for similar masses. One possible explanation for this density spread is giant collisions stripping planets of their atmospheres. In this paper we present the results from a series of smoothed particle hydrodynamics (SPH) simulations of head-on collisions of planets with significant atmospheres and bare projectiles without atmospheres. Collisions between planets can have sufficient energy to remove substantial fractions of the mass from the target planet. We find the fraction of mass lost splits into two regimes -- at low impact energies only the outer layers are ejected corresponding to atmosphere dominated loss, at higher energies material deeper in the potential is excavated resulting in significant core and mantle loss. Mass removal is less efficient in the atmosphere loss dominated regime compared to the core and mantle loss regime, due to the higher compressibility of atmosphere relative to core and mantle. We find roughly twenty per cent atmosphere remains at the transition between the two regimes. We find that the specific energy of this transition scales linearly with the ratio of projectile to target mass for all projectile-target mass ratios measured. The fraction of atmosphere lost is well approximated by a quadratic in terms of the ratio of specific energy and transition energy. We provide algorithms for the incorporation of our scaling law into future numerical studies.