Varadi et al. (2003) and Laskar et al. (2011). These authors have performed long-term numerical simulations of the orbits of the major planets in our Solar System using a variety of models and integration algorithms. It is obvious that the precision of our present astronomical computations within the simulated time frame is comparable to that in these recent studies as seen in Fig. \[validation\]. The figure does not show any large differences between our results and those of Varadi et al. (2003) or Laskar et al. (2011). There are no unusual features that would hint at a major problem with our models or integration method. Here, the results of Varadi et al. (2003) paper have been obtained from Prof. Varadi’s web site[^8]. The data of Laskar et al. (2011) have been downloaded from the Astronomical Solutions for Earth paleoclimates web site[^9]. We interpret these positive comparisons as an explicit validation of our calculations.

Results
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The Venus quasi-satellite 2002 VE$_{68}$ is an unusual object that is directly perturbed by three of the inner planets, Mercury, Venus and the Earth. The object has a very significant eccentricity (0.41) and it is an obvious candidate to be in an unstable orbit. The 