This article is about orbits in celestial mechanics, due to gravity. For other uses, see Orbit (disambiguation).
An animation showing a low eccentricity orbit (near-circle, in red), and a high eccentricity orbit (ellipse, in purple)
In celestial mechanics, an orbit (also known as orbital revolution) is the curved trajectory of an object[1] such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and satellites follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse,[2] as described by Kepler's laws of planetary motion.
For most situations, orbital motion is adequately approximated by Newtonian mechanics, which explains gravity as a force obeying an inverse-square law.[3] However, Albert Einstein's general theory of relativity, which accounts for gravity as due to curvature of spacetime, with orbits following geodesics, provides a more accurate calculation and understanding of the exact mechanics of orbital motion.
^"orbit (astronomy)". Encyclopædia Britannica (Online ed.). Archived from the original on 5 May 2015. Retrieved 28 July 2008.
^"The Space Place :: What's a Barycenter". NASA. Archived from the original on 8 January 2013. Retrieved 26 November 2012.
^Kuhn, The Copernican Revolution, pp. 238, 246–252
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