The Quasi-Satellite Orbit: Theory and Examples

Details The Quasi-Satellite Orbit: Theory and Examples The Quasi-Satellite Orbit: Theory and Examples

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dda....37.1501w&link_type=abstract

American Astronomical Society, DDA meeting #37, #15.01; Bulletin of the American Astronomical Society, Vol. 38, p.676

Astronomy and Astrophysics

Astronomy

Scientific paper

An asteroid moving around the Sun having the same mean motion and mean longitude as a planet, but a different eccentricity, remains near the planet much like a satellite even when the distance is large enough so that it is not a bound satellite in the strictest sense (eg. even when it is well outside the planet's Hill sphere). This motion, which we term "quasi-satellite" (QS) motion, is one class of possible behaviours of small bodies in 1:1 mean-motion resonance with a planet, of which Trojan or tadpole motion is perhaps the best known class. If the QS orbit is coplanar with the planet, then the motion is stable in the secular approximation. When the orbits are inclined enough, an asteroid can be trapped into such a quasi-satellite (QS) motion for a finite period of time. The conditions under which this can occur are discussed and examples of recently-discovered QS objects in our own Solar System are examined.
This work was supported in part by the Natural Sciences and Engineering Research Council of Canada.

Affiliated with

Also associated with

No associations

Rating

The Quasi-Satellite Orbit: Theory and Examples does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The Quasi-Satellite Orbit: Theory and Examples, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Quasi-Satellite Orbit: Theory and Examples will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1059103