DYNAMICS OF EROS

We have investigated the dynamical evolution of asteroid (433) Eros, s oon to be explored by the Near-Earth Asteroid Rendezvous (NEAR) probe, by performing 16 numerical integrations of ''dynamical clones'' of Er os's chaotic orbit over a timespan of 5 Myr. By analyzing the results of these integrations we have found the following: (1) In six cases a clone becomes an Earth crosser, typically because of eccentricity incr eases caused by the nu(3) and nu(4) secular resonances; two clones bec ome Venus crossers, and one eventually collides with the Sun. (2) Some of the Earth-crossing clones go back to the Mars-crossing state after some time, and several have their inclination affected by the nu(13) and nu(14) nodal resonances. (3) Nine clones have a slow evolution dom inated by Mars encounters, and one of them is temporarily trapped into the 25:24 mean motion resonance with Mars, providing effective protec tion from close encounters over more than I Myr. (4) From the number o f planetary encounters recorded during our integrations, Eros's lifeti me versus a collision with Earth and Mars can be estimated to be about 1.84 and 2.9 Gyr, respectively. (5) On the other hand, it is impossib le to estimate even as an order of magnitude the past or future mean i mpact rate onto Eros's surface. These findings have the following impl ications: Eros's dynamical lifetime is probably of the order of 50-100 Myr, and it has approximate to 5% probability of eventually hitting E arth. Its shape may have been affected by tidal forces during past Ear th encounters. Its birth location in the main belt cannot be traced ba ck with certainty, but if Eros comes from a family-forming catastrophi c breakup near one of the main resonances, this must have been one of the last such events to occur in the main belt. More likely, Eros's or bit became Mars crossing by slowly diffusing from the high-eccentricit y portion of the main belt; then, Mars and Earth encounters led it to its current state. Unfortunately, the forthcoming observations of Eros 's cratering record by the NEAR probe will not be useful to constrain its age or collisional lifetime.