An orbital pole is either point at the ends of the orbital normal, an imaginary line segment that runs through a focus of an orbit (of a revolving body like a planet, moon or satellite) and is perpendicular (or normal) to the orbital plane. Projected onto the celestial sphere, orbital poles are similar in concept to celestial poles, but are based on the body's orbit instead of its equator.
The north orbital pole of a revolving body is defined by the right-hand rule. If the fingers of the right hand are curved along the direction of orbital motion, with the thumb extended and oriented to be parallel to the orbital axis, then the direction the thumb points is defined to be the orbital north.
The poles of Earth's orbit are referred to as the ecliptic poles. For the remaining planets, the orbital pole in ecliptic coordinates is given by the longitude of the ascending node (☊) and inclination (i): l = ☊ - 90°, b = 90° - i. In the following table, the planetary orbit poles are given in both celestial coordinates and the ecliptic coordinates for the Earth.
When a satellite orbits close to another large body, it can only maintain continuous observations in areas near its orbital poles. The continuous viewing zone (CVZ) of the Hubble Space Telescope lies inside roughly 24° of Hubble's orbital poles, which precess around the Earth's axis every 56 days.
The ecliptic is the plane on which Earth orbits the Sun. The ecliptic poles are the two points where the ecliptic axis, the imaginary line perpendicular to the ecliptic, intersects the celestial sphere.
The two ecliptic poles are mapped below.
Due to axial precession, either celestial pole completes a circuit around the nearer ecliptic pole every 25,800 years.
the positions of the ecliptic poles expressed in equatorial coordinates, as a consequence of Earth's axial tilt, are the following:
North: right ascension (exact), declination
South: right ascension (exact), declination
The North Ecliptic Pole is located near the Cat's Eye Nebula and the South Ecliptic Pole is located near the Large Magellanic Cloud.
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The poles of astronomical bodies are determined based on their axis of rotation in relation to the celestial poles of the celestial sphere. Astronomical bodies include stars, planets, dwarf planets and small Solar System bodies such as comets and minor planets (e.g., asteroids), as well as natural satellites and minor-planet moons. Axial tilt The International Astronomical Union (IAU) defines the north pole of a planet or any of its satellites in the Solar System as the planetary pole that is in the same celestial hemisphere, relative to the invariable plane of the Solar System, as Earth's north pole.
vignette|Le satellite (rouge) est rétrograde car il orbite dans la direction opposée à la rotation de sa planète (bleu/noir). vignette|Dans cette animation, le satellite orange décrit un mouvement rétrograde autour de sa planète, contrairement aux trois autres.
Éris, officiellement (136199) Éris (internationalement 136199 Eris ; désignation provisoire ), est une planète naine du Système solaire, la plus massive (27 % de plus que Pluton) et la deuxième plus grande ( de diamètre, contre pour Pluton). C'est ainsi le connu le plus massif et le plus grand en orbite directement autour du Soleil. Par ailleurs, c'est le plus gros objet du Système solaire n'ayant pas encore été survolé par une sonde spatiale. Objet transneptunien, et plus précisément un objet du disque des objets épars, Éris est située au-delà de la ceinture de Kuiper.
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