The JADE code: Coupling secular exoplanetary dynamics and photo-evaporation

TL;DR

The paper introduces the JADE code, a tool that couples secular orbital dynamics and atmospheric photo-evaporation to better understand the evolution of close-in exoplanets, especially in the context of migration and atmospheric loss.

Contribution

The JADE code uniquely integrates secular orbital evolution with atmospheric escape processes, enabling high-precision simulations of exoplanet evolution over long timescales.

Findings

Confirmed Kozai migration explains GJ436 b's orbit.

Discovered atmospheric pulsations linked to Kozai cycles.

Identified delayed evaporation as a key factor in the hot Neptune desert edge.

Abstract

Close-in planets evolve under extreme conditions, raising questions about their origins and current nature. Two predominant mechanisms are orbital migration, which brings them close to their star, and atmospheric escape under the resulting increased irradiation. Yet, their relative roles remain unclear because we lack models that couple the two mechanisms with high precision on secular timescales. To address this need, we developed the JADE code, which simulates the secular atmospheric and dynamical evolution of a planet around its star, and can include the perturbation induced by a distant third body. On the dynamical side, the 3D evolution of the orbit is modeled under stellar and planetary tidal forces, a relativistic correction, and the action of the distant perturber. On the atmospheric side, the vertical structure of the atmosphere is integrated over time based on its thermodynamical properties, inner heating, and the evolving stellar irradiation, which results, in particular, in photo-evaporation. The JADE code is benchmarked on GJ436 b, prototype of evaporating giants on eccentric, misaligned orbits at the edge of the hot Neptunes desert. We confirm that its orbital architecture is well explained by Kozai migration and unveil a strong interplay between its atmospheric and orbital evolution. During the resonance phase, the atmosphere pulsates in tune with the Kozai cycles, which leads to stronger tides and an earlier migration. This triggers a strong evaporation several Gyr after the planet formed, refining the paradigm that mass loss is dominant in the early age of close-in planets. This suggests that the edge of the desert could be formed of warm Neptunes whose evaporation was delayed by migration. It strengthens the importance of coupling atmospheric and dynamical evolution over secular timescales, which the JADE code will allow simulating for a wide range of systems.