argument of periapsis
Όρισμα του περιηλίου
periapsis oor Grieks
periapsis
en
(astronomy) The point of a body's elliptical orbit about the system's centre of mass where the distance between the body and the centre of mass is at its minimum. In the case of other celestial bodies, specialised terms are used. See Apsis (Wikipedia) for details.
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περίαψη
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The eccentricity, e, and either the semi-major axis, a, or the distance of periapsis, q, are used to specify the shape and size of an orbit.
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The most appreciable changes in their orbits occur approximately every 6.2 years, when the periapsis of Pandora lines up with the apoapsis of Prometheus and the moons approach to within about 1,400 kilometres (870 mi).
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The anomalistic period is the time that elapses between two passages of an object at its periapsis (in the case of the planets in the Solar System, called the perihelion), the point of its closest approach to the attracting body.
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In all cases, the direction of A lies along the symmetry axis of the conic section and points from the center of force toward the periapsis, the point of closest approach.
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Scientific instruments were generally turned on for about 30 minutes near periapsis.
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From Venus orbit insertion to July 1980, periapsis was held between 142 and 253 kilometres (88 and 157 mi) (at 17 degrees north latitude) to facilitate radar and ionospheric measurements.
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Thereafter, the periapsis was allowed to rise to a maximum of 2,290 kilometres (1,420 mi) and then fall, to conserve fuel.
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Periapsis is used to calculate the trajectory of a celestial body entering the atmosphere of a planet's gravitational field.
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Adding the argument of periapsis to the longitude of the ascending node gives the longitude of the periapsis.
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Argument of periapsis - Wikipedia
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