The dynamics of the TRAPPIST-1 system in the context of its formation

TL;DR

This study uses N-body simulations to test if sequential planet formation and migration can produce the current resonant configuration of the TRAPPIST-1 system, highlighting the importance of crossing the migration barrier.

Contribution

It demonstrates that crossing the migration barrier is necessary for reproducing the observed higher-order resonances in TRAPPIST-1, supporting the sequential formation model.

Findings

Sequential migration naturally forms a chain of first-order resonances.

Crossing the migration barrier is crucial for matching observed period ratios.

Early cavity infall scenario aligns best with the current system configuration.

Abstract

TRAPPIST-1 is an 0.09 $M_{\odot}$ star, which harbours a system of seven Earth-sized planets. Two main features stand out: (i) all planets have similar radii, masses, and compositions; and (ii) all planets are in resonance. Previous works have outlined a pebble-driven formation scenario where planets of similar composition form sequentially at the H$_2$O snowline (${\sim}0.1$ au for this low-mass star). It was hypothesized that the subsequent formation and migration led to the current resonant configuration. Here, we investigate whether the sequential planet formation model is indeed capable to produce the present-day resonant configuration, characterized by its two-body and three-body mean motion resonances structure. We carry out N-body simulations, accounting for type-I migration, stellar tidal damping, disc eccentricity-damping, and featuring a migration barrier located at the disc's inner edge. Due to the sequential migration, planets naturally form a chain of first-order resonances. But to explain the period ratios of the b/c/d-system, which are presently in higher-order resonances, we find that planets b and c must have marched across the migration barrier, into the gas-free cavity, before the disc has dispersed. We investigate both an early and late cavity infall scenario and find that the early infall model best matches the constraints, as well as being more probable. After the dispersal of the gaseous disc, stellar tidal torque also contributes towards a modest separation of the inner system. We outline how the insights obtained in this work can be applied to aid the understanding of other compact resonant planet systems.