Finite-Sized Orbiter’s Motion around the Natural Moons of Planets with Slow-Variable Eccentricity of Their Orbit in ER3BP

This article is devoted to the study of stability movement a satellite finite size around natural satellites planets in solar system, using new concept ER3BP with variable eccentricity. was introduced earlier for spin state secondary planet correlated implicitly motion its trapped orbit near (which involved Kepler duet “Sun-planet”). But it real interest explore another kind this problem, plane “planet-moon-satellite”. Here, we consider two primary celestial bodies, and moon, latter revolves common barycenter quasi-elliptical fixed (invariable plane) slowly varying eccentricity on large time scale due tidal phenomena. presents both theoretical numerical results various cases “planet-moon-satellite” trio.