11-129 Jacques Fejoz, Marcel Guardia, Vadim Kaloshin, Pablo Roldan

Diffusion along mean motion resonance in the restricted planar three-body problem (2938K, Postscript) Sep 12, 11

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Abstract. We study the dynamics of the restricted planar three-body problem near a mean motion resonance, i.e. a resonance involving the Keplerian periods of the two lighter bodies revolving around the most massive one. This problem is often used to model Sun--Jupiter--asteroid systems. For the primaries (Sun and Jupiter), we pick a realistic mass ratio $\mu=10^{-3}$ and a small eccentricity $e_0>0$. The main result is a construction of a variety of diffusing orbits which show a drastic change of the osculating eccentricity of the asteroid, while the osculating semi major axis is kept almost constant. The proof relies on the careful analysis of the circular problem, which has a hyperbolic structure, but for which diffusion is prevented by KAM tori. In the proof we verify certain non-degeneracy conditions numerically. Based on the work of Treschev, it is natural to conjecture that the time of diffusion for this problem is at least $\sim -\ln (\mu e_0)/ (\mu^{3/2} e_0)$. We expect our instability mechanism to apply to realistic values of $e_0$ and we give heuristic arguments in its favor. If so, the applicability of Nekhoroshev theory to the three-body problem as well as the long time stability become questionable. It is well known that, in the Asteroid Belt, located between the orbits of Mars and Jupiter, the distribution of asteroids has the so-called {\it Kirkwood gaps} exactly at mean motion resonances of low order. Our mechanism gives a possible explanation of their existence. To relate the existence of Kirkwood gaps with Arnold diffusion, we also state a conjecture on its existence for a typical $\eps$-perturbation of the product of the pendulum and the rotator. Namely, we predict that a positive conditional measure of initial conditions concentrated in the main resonance exhibits Arnold diffusion on time scales $- \ln \eps / \eps^{2}$.

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