Mercury’s Chaotic Secular Evolution as a Subdiffusive Process

Abstract

Mercury’s orbit can destabilize, generally resulting in a collision with either Venus or the Sun. Chaotic evolution can cause g _1 to decrease to the approximately constant value of g _5 and create a resonance. Previous work has approximated the variation in g _1 as stochastic diffusion, which leads to a phenomological model that can reproduce the Mercury instability statistics of secular and N -body models on timescales longer than 10 Gyr. Here we show that the diffusive model significantly underpredicts the Mercury instability probability on timescales less than 5 Gyr, the remaining lifespan of the solar system. This is because g _1 exhibits larger variations on short timescales than the diffusive model would suggest. To better model the variations on short timescales, we build a new subdiffusive phenomological model for g _1 . Subdiffusion is similar to diffusion but exhibits larger displacements on short timescales and smaller displacements on long timescales. We choose model parameters based on the behavior of the g _1 trajectories in the N -body simulations, leading to a tuned model that can reproduce Mercury instability statistics from 1–40 Gyr. This work motivates fundamental questions in solar system dynamics: why does subdiffusion better approximate the variation in g _1 than standard diffusion? Why is there an upper bound on g _1 , but not a lower bound that would prevent it from reaching g _5 ?

Keywords

• Mercury (planet)
• Planetary dynamics