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Also, when Achilles and Hector were about to engage in a fight to the death, the god Zeus weighed both warriors' keres to determine who shall die. [7] As Hector’s ker was deemed heavier, he was the one destined to die and in the weighing of souls, Zeus chooses Hector to be killed. [8] During the festival known as Anthesteria, the Keres were ...
In celestial mechanics, the argument of latitude is an angular parameter that defines the position of a body moving along a Kepler orbit. It is the angle between the ascending node and the body. It is the sum of the more commonly used true anomaly and argument of periapsis .
In celestial mechanics, true anomaly is an angular parameter that defines the position of a body moving along a Keplerian orbit. It is the angle between the direction of periapsis and the current position of the body, as seen from the main focus of the ellipse (the point around which the object orbits).
On the computation of the eccentric anomaly, equation of the centre and radius vector of a planet, in terms of the mean anomaly and eccentricity. Monthly Notices of the Royal Astronomical Society, Vol. 43, p. 345. Gives the equation of the center to order e 12. Morrison, J. (1883). Errata. Monthly Notices of the Royal Astronomical Society, Vol ...
Instead of the mean anomaly at epoch, the mean anomaly M, mean longitude, true anomaly ν 0, or (rarely) the eccentric anomaly might be used. Using, for example, the "mean anomaly" instead of "mean anomaly at epoch" means that time t must be specified as a seventh orbital element. Sometimes it is assumed that mean anomaly is zero at the epoch ...
The name celestial mechanics is more recent than that. Newton wrote that the field should be called "rational mechanics". Newton wrote that the field should be called "rational mechanics". The term "dynamics" came in a little later with Gottfried Leibniz , and over a century after Newton, Pierre-Simon Laplace introduced the term celestial ...
In celestial mechanics, a Kepler orbit (or Keplerian orbit, named after the German astronomer Johannes Kepler) is the motion of one body relative to another, as an ellipse, parabola, or hyperbola, which forms a two-dimensional orbital plane in three-dimensional space. A Kepler orbit can also form a straight line.
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.