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The apsides refer to the farthest (2) and nearest (3) points reached by an orbiting planetary body (2 and 3) with respect to a primary, or host, body (1). An apsis (from Ancient Greek ἁψίς (hapsís) 'arch, vault'; pl. apsides / ˈ æ p s ɪ ˌ d iː z / AP-sih-deez) [1] [2] is the farthest or nearest point in the orbit of a planetary body about its primary body.
a (km) is the average orbital distance between the centers of the two bodies; r 1 (km) is the distance from the center of the primary to the barycenter; R 1 (km) is the radius of the primary r 1 / R 1 a value less than one means the barycenter lies inside the primary
At θ = 90° and at θ = 270° the distance is equal to . At θ = 180°, aphelion, the distance is maximum (by definition, aphelion is – invariably – perihelion plus 180°) = The semi-major axis a is the arithmetic mean between r min and r max:
r a is the radius at apoapsis (also "apofocus", "aphelion", "apogee"), i.e., the farthest distance of the orbit to the center of mass of the system, which is a focus of the ellipse. r p is the radius at periapsis (or "perifocus" etc.), the closest distance.
Some of these TNOs with an extreme aphelion are detached objects such as 2010 GB 174, which always reside in the outermost region of the Solar System, while for other TNOs, the extreme aphelion is due to an exceptionally high eccentricity such as for 2005 VX 3, which orbits the Sun at a distance between 4.1 (closer than Jupiter) and 2200 AU (70 ...
is the distance of the orbiting body from the central body, is the length of the semi-major axis, is the standard gravitational parameter. Conclusions: For a given semi-major axis the specific orbital energy is independent of the eccentricity. Using the virial theorem to find:
In gravitationally bound systems, the orbital speed of an astronomical body or object (e.g. planet, moon, artificial satellite, spacecraft, or star) is the speed at which it orbits around either the barycenter (the combined center of mass) or, if one body is much more massive than the other bodies of the system combined, its speed relative to the center of mass of the most massive body.
Leleākūhonua orbits the Sun at a distance varying from 65 to about 2000 AU once roughly every 32,000 years (semi-major axis of around 1000–1200 AU).Its orbit has a very high eccentricity of 0.94 and an inclination of 12° with respect to the ecliptic. [4]