Franco-Rodriguez, Jorge Adalberto
June 24, 2014
Gravitational Two-Body problem, Three-Body problem, N-Body problem, Solar System.
The prediction of the movement of a group of N gravitationally attracting bodies around its center of mass CM, given their initial positions and velocities, was successfully undertaken in previous papers. In order to sketch those elliptic and considered stable motions, obtained equations of orbits were put in function of their semi-major axis. This presentation simplified the geometric consideration of initial conditions. This work is the continuation of the previous representation of gravitational bodies’ paths, but now applying the nested two-body type configurations as one of the possible arrangements allowed by Newton Equations under the optics of the solution of the N-Body Problem presented in previous papers demonstrating an explanation of the stability of the Solar System.