Run a live three-body simulation in your browser. Edit masses, 3D positions and velocities, then track trajectories, energy, angular momentum and center-of-mass drift.
Newtonian point masses. No relativity, collisions, tides or finite radii. Softening replaces r with √(r²+ε²) near close encounters.
Units follow your chosen numbers. Figure-8/Lagrange/Burrau use normalized units; the Solar preset uses solar masses, AU and years.
All calculations and animation run locally in your browser.
Numerically integrates three point masses under Newtonian gravity. Choose Velocity Verlet or RK4; a softening parameter regularizes very close encounters.
No. The general three-body problem has no general closed-form solution; this tool numerically integrates the equations of motion through time.
Velocity Verlet is a strong default for long orbital runs because of its symplectic behavior. RK4 is useful for accurate short runs but is not symplectic.
A timestep that is too large or a very close encounter can increase numerical error. Reduce dt and, if appropriate, use a small softening value.
No. The simulation and rendering run entirely in your browser.
