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Classical central-force problem : ウィキペディア英語版 | Classical central-force problem In classical mechanics, the central-force problem is to determine the motion of a particle under the influence of a single central force. A central force is a force that points from the particle directly towards (or directly away from) a fixed point in space, the center, and whose magnitude only depends on the distance of the object to the center. In many important cases, the problem can be solved analytically, i.e., in terms of well-studied functions such as trigonometric functions. The solution of this problem is important to classical physics, since many naturally occurring forces are central. Examples include gravity and electromagnetism as described by Newton's law of universal gravitation and Coulomb's law, respectively. The problem is also important because some more complicated problems in classical physics (such as the two-body problem with forces along the line connecting the two bodies) can be reduced to a central-force problem. Finally, the solution to the central-force problem often makes a good initial approximation of the true motion, as in calculating the motion of the planets in the Solar System.
==Basics==
The essence of the central-force problem is to solve for the position r〔Throughout this article, boldface type is used to indicate that quantities such as r and F are vectors, whereas ordinary numbers are written in italics. Briefly, a vector v is a quantity that has a magnitude ''v'' (also written |v|) and a direction. Vectors are often specified by their components. For example, the position vector r = (''x'', ''y'') in Cartesian coordinates is described as an ordered pair of its ''x'' and ''y'' coordinates.〕 of a particle moving under the influence of a central force F, either as a function of time ''t'' or as a function of the angle φ relative to the center of force and an arbitrary axis.
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