osculating orbit


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osculating orbit

(os -kyŭ-layt-ing) The truly elliptical orbit that a celestial object would follow if the perturbing forces of other bodies were to disappear so that it was subject only to the central gravitational field of a single massive body. In general elliptical motion is an approximation to the real motion of members of the Solar System. If all forces except the central gravitational force disappeared at time t , then the osculating elements would be the orbital elements of the ellipse followed by a body at a given instant after time t . For a real body in perturbed motion the instantaneous osculating elements are not constant but are functions of time. The osculating elements are often used to describe the perturbed motion of a body.

Osculating Orbit

 

the orbit that a celestial body would assume if at some instant in time the body were freed from all perturbing forces. An osculating orbit can be determined for any instant, and in general, different osculating orbits correspond to different instants. The elements that determine an osculating orbit are called osculating elements, and the instant for which these elements are computed is called the instant of osculation. An osculating orbit may be an ellipse, parabola, or hyperbola, and one that is calculated for an instant in the middle of a period of observation very closely corresponds to the actual motion of a celestial body over a certain length of time; in the case of a small planet or comet, this length of time can be several weeks or even months.

The actual motion of a celestial body may be considered as motion along an osculating orbit whose elements change continuously with time. Thus, at the instant of osculation the osculating orbit touches on the actual trajectory of the body, and for this reason it is also called the instantaneous orbit. Although osculating orbits may be used to study any type of orbital motion, their application in the method of variation of parameters (which in this case are the osculating elements) is most effective when the perturbing forces are small compared with the attraction of the central body. The fundamentals of the method of variation of parameters were first presented by I. Newton, and this method was later worked out in detail by J. Lagrange.

REFERENCES

Lagrange, J. Analiticheskaia mekhanika, vols. 1–2. Moscow-Leningrad, 1950. (Translated from French.)

G. A. CHEBOTAREV

osculating orbit

[′äs·kyə‚lād·iŋ ′ȯr·bət]
(astronomy)
The orbit which would be followed by a body such as an asteroid or comet if, at a given time, all the planets suddenly disappeared, and it then moved under the gravitational force of the sun alone.