This lies for the most part inside the Earth's orbit, which it crosses near the asteroid's furthest point from the Sun, the aphelion.

The most numerous known co-orbital asteroids are the so-called trojans, which occupy the L4 and L5 Lagrangian points of the relevant planet.

This spiral motion (in the Earth–Sun reference frame) arises from the slightly lower eccentricity and the tilt of the orbit: the inclination relative to the Earth's orbit is responsible for the vertical component of the spiral loop, and the difference in eccentricity for the horizontal component.

Again it comes under the Earth's gravitational influence; this time it is lifted onto a slower orbit, further from the Sun.

Calculations indicate that in the next few thousand years it will never come closer than 4.5 million kilometres, or about twelve times the distance from the Earth to the Moon.

Because it is not bound to the Earth like the Moon but is mainly under the gravitational influence of the Sun, it belongs to the bodies called quasi-satellites.

Because of its nearness to the Sun, it cannot however consist of volatile substances such as water ice, since these would evaporate or sublime; one can clearly observe this happening to a comet as this forms the visible tail.

[5] Using radar echo measurements at the Arecibo radio telescope the rotational period of 2002 AA29 could be determined.

This rapid rotation together with the small diameter and therefore low mass leads to some interesting conclusions: Because its orbit is very similar to the Earth's, the asteroid is relatively easily reachable by space probes.

2002 AA29 would therefore be a suitable object of study for more precise research into the structure and formation of asteroids and the evolution of their orbits around the Sun.

Furthermore, it is assumed that there are small trojan companions of the Earth with diameters in the region of 100 metres located at the L4 and L5 Lagrangian points of the Earth–Sun system.