System Architecture and Planetary Obliquity: Implications for Long-Term Habitability

TL;DR

This study investigates how the architecture of planetary systems, especially the presence and characteristics of giant planets, influences the long-term habitability of Earth-like planets through orbital and climate dynamics.

Contribution

It demonstrates the impact of giant planet orbital properties on the eccentricity, obliquity, and climate cycles of Earth-like planets, highlighting factors that enhance or reduce habitability.

Findings

Higher eccentricity of a giant planet can increase habitability if obliquity remains low.

Closer giant companions lead to shorter eccentricity cycles but longer obliquity cycles.

Obliquity cycle characteristics are linked to orbital inclination and precession.

Abstract

In the search for life beyond our Solar system, attention should be focused on those planets that have the potential to maintain habitable conditions over the prolonged periods of time needed for the emergence and expansion of life as we know it. The observable planetary architecture is one of the determinants for long-term habitability as it controls the orbital evolution and ultimately the stellar fluxes received by the planet. With an ensemble of n-body simulations and obliquity models of hypothetical planetary systems, we demonstrate that the amplitude and period of eccentricity, obliquity, and precession cycles of an Earth-like planet are sensitive to the orbital characteristics of a giant companion planet. A series of transient, ocean-coupled climate simulations show how these characteristics of astronomical cycles are decisive for the evolving surface conditions and long-term fractional habitability relative to the modern Earth. The habitability of Earth-like planets increases with the eccentricity of a Jupiter-like companion, provided that the mean obliquity is sufficiently low to maintain temperate temperatures over large parts of its surface throughout the orbital year. A giant companion closer in results in shorter eccentricity cycles of an Earth-like planet but longer, high-amplitude, obliquity cycles. The period and amplitude of obliquity cycles can be estimated to first order from the orbital pathways calculated by the n-body simulations. In the majority of simulations, obliquity amplitude relates directly to the orbital inclination whereas the period of obliquity cycles is a function of nodal precession and the proximity of a giant companion.