remained for some time in the 1:1 mean motion resonance with Venus alternating among the various resonant states: $L_{5}$ Trojan, $L_{4}$ Trojan (tadpole orbits), horseshoe orbit, quasi-satellite or combinations of two or more of these orbits (some of them not displayed).

As expected for an object moving in a rather eccentric orbit and submitted to the direct perturbation of multiple planets, its orbit is certainly unstable. The orbital elements of 2002 VE$_{68}$ are plotted in Fig. \[orbele1\]. When the object enters the quasi-satellite dynamical state, the eccentricity increases, the inclination decreases and the value of the semi-major axis remains almost constant oscillating around the value of the semi-major axis of Venus. Large variations in both eccentricity and inclination are observed when the object goes from the $L_{5}$ Lagrangian point to $L_{4}$.

Transitions between the various resonant phases are triggered by close encounters with planets: the object is a Mercury grazer, Venus crosser and Earth crosser. In Fig. \[distance1\] we show that the distance of 2002 VE$_{68}$ from Venus remains larger than 0.1 AU until the object is ejected from the quasi-satellite dynamical state into the $L_{5}$ Lagrangian point to become a Venus Trojan about 500 yr from now. Encounters with 