Secular models and Kozai resonance for planets in coorbital non-coplanar motion

TL;DR

This paper develops analytical and semi-analytical secular models for coorbital non-coplanar planetary systems, comparing them with numerical simulations and exploring stability and resonance phenomena like Kozai and Lidov-Kozai effects.

Contribution

It introduces new models for coorbital planetary dynamics that work across a wide range of eccentricities and inclinations, extending understanding of stability and resonance.

Findings

Analytical model accurately replicates N-body simulations for moderate eccentricities and inclinations.

Semianalytical model valid for any coorbital configuration, eccentricity, and inclination.

Discovery of stable Earth-like planet orbits in previously unstable regions.

Abstract

In this work, we construct and test an analytical and a semianalytical secular models for two planets locked in a coorbital non-coplanar motion, comparing some results with the case of restricted three body problem. The analytical average model replicates the numerical N-body integrations, even for moderate eccentricities ($\lesssim$ 0.3) and inclinations ($\lesssim10^\circ$), except for the regions corresponding to quasi-satellite and Lidov-Kozai configurations. Furthermore, this model is also useful in the restricted three body problem, assuming very low mass ratio between the planets. We also describe a four-degree-of-freedom semianalytical model valid for any type of coorbital configuration in a wide range of eccentricities and inclinations. {Using a N-body integrator, we have found that the phase space of the General Three Body Problem is different to the restricted case for inclined systems, and establish the location of the Lidov-Kozai equilibrium configurations depending on mass ratio. We study the stability of periodic orbits in the inclined systems, and find that apart from the robust configurations $L_4$, $AL_4$, and $QS$ is possible to harbour two Earth-like planets in orbits previously identified as unstable $U$ and also in Euler $L_3$ configurations, with bounded chaos.