A numerical method to solve a three-body problem involves using numerical integrators to evolve the system's equations of motion, typically due to gravitational forces. The complexity arises because the equations are not separable, necessitating iterative solutions like Euler's method. Examples include the Sun, Earth, and Moon system, where gravitational interactions complicate the motion of celestial bodies. The discussion also touches on the transition from a three-body to a two-body problem based on mass and distance, questioning whether proximity or physical contact alters the classification. Ultimately, the determination of whether a system is a three-body or two-body problem can depend on specific conditions and subjective judgment.