2012-Sep-30.0; J2000.0 ecliptic and equinox.) Values include the 1-$\sigma$ uncertainty (Source: JPL Small-Body Database).

\[elements\]

2002 VE$_{68}$: current dynamical status
----------------------------------------

2002 VE$_{68}$ was identified as quasi-satellite of Venus by Mikkola et al. (2004). It was the first quasi-satellite observed and identified as such. The quasi-satellite dynamical state is a specific configuration of the 1:1 mean motion resonance with a host planet in which the object appears to travel around the planet but is not gravitationally bound to it: the body librates around the longitude of its associated planet but its trajectory is not closed. The term “quasi-satellite” was first used in a scientific paper by Danielsson & Ip (1972a) in the context of explaining the resonant behaviour of the NEO (1685) Toro with the Earth (Danielsson & Ip 1972b). However, this early mention was not directly connected with the topic of co-orbital bodies and it is usually considered that the term was first introduced and popularized among the scientific community by Mikkola & Innanen (1997), although the concept behind it was initially studied by Jackson (1913) and the energy balance associated to the resonant state was first analyzed by Hénon (1969). Further analysis was carried out by Szebehely (1967), 