Three-body problem

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

The three-body problem is a problem in the field of physics that experts find interesting. It would be for instance the problem of the movement of the Sun, the Earth and the Moon.

What experts call "non-relativistic movement"[change | change source]

"relativistic" refers to the theory of Albert Einstein called Relativity. This theory must be used when things move at great speed. But as long as things move at small enough speed, you can use every day classical mechanics, and this is called "non-relativistic movement". You know if the speed is great or small enough by comparing to the speed of light c which is the highest possible speed.

Differences between "relativistic" and "non-relativistic"[change | change source]

When a thing is moving, it has energy of movement. Scientists use a short-cut when they talk about this energy, they call it 'E.'

In a field called classical mechanics, experts say that movement with higher velocities causes the radiation of gravitational waves. In this case, the thing moving lose energy, and this make calculation more difficult. Experts say that the system is "not conservative".

Experts in another field called quantum mechanics, say, in addition, at high speed the creation and annihilation of particles becomes possible, so, it is not possible to keep the number of particles constant.

In astronomy[change | change source]

The three-body problem also happens in astronomy. The problem consists in calculating the course of three bodies, that influence each other with gravitation. The first to state the problem was Isaac Newton, in Principia. Usually, two of the bodies are large, and the third is small. In the case where the two bodies have the same gravitational force, and that the bodies all have the same mass can be solved exactly. If this is not the case, the problem is solved through iteration and approximation.