Dynamical Evolution of NEAs: Close Encounters, Secular Perturbations and Resonances

Details Dynamical Evolution of NEAs: Close Encounters, Secular Perturbations and Resonances Dynamical Evolution of NEAs: Close Encounters, Secular Perturbations and Resonances

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996em%26p...72..151m&link_type=abstract

Earth, Moon and Planets, Volume 72, Issue 1-3, pp. 151-164

Computer Science

15

Near-Earth Asteroids, Resonances, Close Encounters

Scientific paper

We discuss the main mechanisms affecting the dynamical evolution of Near-Earth Asteroids (NEAs) by analyzing the results of three numerical integrations over 1 Myr of the NEA (4179) Toutatis. In the first integration the only perturbing planet is the Earth. So the evolution is dominated by close encounters and looks like a random walk in semimajor axis and a correlated random walk in eccentricity, keeping almost constant the perihelion distance and the Tisserand invariant. In the second integration Jupiter and Saturn are present instead of the Earth, and the 3/1 (mean motion) and v 6 (secular) resonances substantially change the eccentricity but not the semimajor axis. The third, most realistic, integration including all the three planets together shows a complex interplay of effects, with close encounters switching the orbit between different resonant states and no approximate conservation of the Tisserand invariant. This shows that simplified 3-body or 4-body models cannot be used to predict the typical evolution patterns and time scales of NEAs, and in particular that resonances provide some “fast-track” dynamical routes from low-eccentricity to very eccentric, planet-crossing orbits.

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