to determine the motion of two point particles that interact only with each other
In classical mechanics, the two-body problem is used 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 perfect spheres that never collide with one another and that all external forces are negligible compared to the force of interaction between the two bodies.
The most prominent example of the classical two-body problem is the gravitational case (see also Kepler problem), arising in astronomy for predicting the orbits (or escapes from orbit) of objects such as satellites, planets, and stars. A two-point-particle model of such a system nearly always describes its behavior well enough to provide useful insights and predictions.
Discovered by embedding cosine similarity (sentence-transformers MiniLM, 384-dim).