Here we revisit the topic of the current dynamical status of this remarkable object as well as look into its dynamical past and explore its future orbital evolution which is driven by close encounters with both the Earth and Mercury. In our calculations we use the most updated ephemerides and include the perturbations by the eight major planets. In addition, we include perturbations from the Moon and the three largest asteroids, (1) Ceres, (2) Pallas and (4) Vesta.

This paper is organized as follows: in Section 2 the details of our numerical integrations are given. In Section 3, we present the results of our simulations. We discuss our results in Section 4. In Section 5 we compare our results with those obtained by Mikkola et al. (2004) and our conclusions are summarized in Section 6.

Simulations
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In our calculations we directly integrate the full equations of motion using the Hermite scheme described by Makino (1991) and Aarseth (2003). Additional simulations were completed using the time-symmetric Hermite method described by Kokubo, Yoshinaga & Makino (1998) but it was found that, for the problem studied here, its overall performance was lower and the results largely identical. The Hermite scheme allows efficient 