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Simulate Keplerian celestial mechanics, N-body gravitational interactions, planetary slingshots, and stable three-body figure-8 orbital choreographies in real time.
All planets move in elliptical orbits with the central star situated at one of the two focal points.
A line segment joining a planet and the Sun sweeps out equal areas during equal intervals of time (dA/dt = constant).
The square of an orbital period is directly proportional to the cube of the semi-major axis: T² ∝ a³.