Abstract
A large fraction (> 30%) of the numbered main-belt asteroids follow chaotic orbits, mainly associated to high-order mean motion resonances (MMRs) either of two-body (asteroid–Jupiter) or three-body type (asteroid–Jupiter–Saturn or Mars). These resonances form a dense network of thin chaotic layers throughout the asteroid belt, where small-amplitude variations in the proper elements of asteroids accumulate slowly over time. This effect is commonly referred to as chaotic diffusion. In this chapter we review recent results on speci?c asteroid groups, whose evolution is governed by an interplay between chaotic di?usion and radial migration, induced by subttle non-gravitational e?ects. In particular, we show how chaotic diffusion leads to the slow dispersion of the Trojan swarms and how long-lived resonant populations of individualy unstable asteroids can be formed and sustained in steady state. Furthermore, we show how simple models of chaotic di?usion can be used to estimate the age of asteroid families. In the second part of this chapter, we review di?erent analytic approaches to the problem of chaotic di?usion in MMRs. The domain of validity of each model is discussed, and a comparison between analytical and numerical results is made. We show that, in the absense of ‘fast’ transport routes, related to secular phenomena, chaotic di?usion in the asteroid belt has a characteristic time-scale of ~ 1 Gy, i.e. the time needed for an asteroid to di?use away from the main belt is of the same order as the age of the solar system.
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Tsiganis, K. (2007). Chaotic Di?usion of Asteroids. In: Benest, D., Froeschle, C., Lega, E. (eds) Topics in Gravitational Dynamics. Lecture Notes in Physics, vol 729. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-540-72984-6_5
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