Evolution of orbits of trans-Neptunian bodies at the 2:3 resonance with Neptune

TL;DR

This study numerically investigates how trans-Neptunian bodies evolve in the 2:3 resonance with Neptune, considering planetary influences, and identifies different orbital behaviors and resonance conditions affecting their stability.

Contribution

It provides new insights into the orbital evolution and resonance interactions of trans-Neptunian objects, including the coexistence of multiple resonances and the influence of initial orbital orientations.

Findings

Bodies leave resonance in about 20 Myr when certain orbital angles decrease.

Longer resonance retention occurs when specific angles increase and decrease.

Regions of eccentricity and inclination favor secular and Kozai resonances, sometimes simultaneously.

Abstract

The results of the numerical investigations of the evolution of orbits of trans-Neptunian bodies at the 2 : 3 resonance with Neptune are presented. The gravitational influence of the four giant planets was taken into account. For identical initial values of the semimajor axes, eccentricities, and inclinations, but for different initial orbital orientations and initial positions in orbits, we obtained different types of variations in the difference {\Delta}{\Omega}={\Omega}-{\Omega}_N in the ascending-node longitudes of the body and Neptune, and in the perihelion argument {\omega}. When {\Delta}{\Omega} decreases and {\omega} increases during evolution, then most of the bodies leave the resonance in 20 Myr. In the case of an increase in {\Delta}{\Omega} and a decrease in {\omega}, the bodies stay in the resonance for a much longer time. Regions of eccentricities and inclinations, for which some bodies were in the {\eta}_18 secular resonance ({\Delta}{\Omega} is almost constant) and in the Kozai resonance ({\omega} is almost constant), were obtained to be larger than those predicted for small variations in the critical angle. Some bodies can at the same time be in both these resonances.