Chaotic diffusion of asteroids in the exterior 1:2 mean motion resonance with Mars

TL;DR

This study investigates how chaotic diffusion near the 1:2 mean motion resonance with Mars affects asteroid dynamics, revealing that resonance can prolong asteroid lifetimes and influence their orbital evolution.

Contribution

The paper provides a systematic analysis of chaotic diffusion near the 1:2 resonance with Mars, highlighting its effects on asteroid eccentricity, inclination, and lifetime in the belt.

Findings

Chaotic diffusion increases orbital dispersion but not mean values.

Resonance mitigates asteroid scattering by Mars at high eccentricities.

Gravitational forces alone cannot account for observed eccentricity changes.

Abstract

The inner asteroid belt between 2.1 and 2.5 au is of particular dynamical significance because it is the dominant source of both chondritic meteorites and near-Earth asteroids. This inner belt is bounded by an eccentricity-type secular resonance and by the 1:3 mean motion resonance with Jupiter. Unless asteroid perihelia are low enough to allow scattering by Mars, escape requires transport to one of the bounding resonances. In addition Yarkovsky forces are generally ineffective in changing either the eccentricity and/or inclination for asteroids with diameter $\gtrsim$30 km. Thus, large asteroids with pericentres far from Mars may only escape from the inner belt through large changes in their eccentricities. In this paper we study chaotic diffusion of orbits near the 1:2 mean motion resonance with Mars in a systematic way. We show that, while chaotic orbital evolution in both resonant and non-resonant orbits increase the dispersion of the inclinations and eccentricities, it does not significantly change their mean values. We show further that, while the dispersive growth is greatest for resonant orbits, at high $e$ the resonance acts to mitigate asteroid scattering by Mars - making the asteroid lifetime in the belt longer than it would have been for a non-resonant orbit. For asteroids of all sizes in both resonant and non-resonant orbits, the changes in eccentricity needed to account for the observations cannot be achieved by gravitational forces alone. The role of resonant trapping in protecting asteroids from encounters with Mars is also analysed.