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In classical mechanics, the two-body problem is to calculate and predict the motion of two massive bodies that are orbiting each other in space. The problem assumes that the two bodies are point particles that interact only with one another; the only force affecting each object arises from the other one, and all other objects are ignored.
Electrostatic potential energy between two bodies in space is obtained from the force exerted by a charge Q on another charge q which is given by = ^, where ^ is a vector of length 1 pointing from Q to q and ε 0 is the vacuum permittivity.
The two-body problem in general relativity (or relativistic two-body problem) is the determination of the motion and gravitational field of two bodies as described by the field equations of general relativity. Solving the Kepler problem is essential to calculate the bending of light by gravity and the motion of a planet orbiting its sun.
The effective potential (also known as effective potential energy) combines multiple, perhaps opposing, effects into a single potential. In its basic form, it is the sum of the 'opposing' centrifugal potential energy with the potential energy of a dynamical system .
In the gravitational two-body problem, the specific orbital energy (or vis-viva energy) of two orbiting bodies is the constant sum of their mutual potential energy and their kinetic energy (), divided by the reduced mass. [1]
For two-body potentials this gradient reduces, thanks to the symmetry with respect to in the potential form, to straightforward differentiation with respect to the interatomic distances . However, for many-body potentials (three-body, four-body, etc.) the differentiation becomes considerably more complex [ 12 ] [ 13 ] since the potential may ...
In physics, an elastic collision is an encounter between two bodies in which the total kinetic energy of the two bodies remains the same. In an ideal, perfectly elastic collision, there is no net loss of kinetic energy into other forms such as heat, noise, or potential energy.
There can be two types of singularities of the n-body problem: collisions of two or more bodies, but for which q(t) (the bodies' positions) remains finite. (In this mathematical sense, a "collision" means that two pointlike bodies have identical positions in space.) singularities in which a collision does not occur, but q(t) does not remain ...