Earth-Moon CR3BP Dynamics
A reproducible CR3BP experiment that computes all five Lagrange points and compares finite-time Monte Carlo dispersion near the unstable L1 and stable L4 regions.
Repository output / project interface01 / Overview
Project overview
The project models the planar circular restricted three-body problem in the Earth-Moon system. It locates the five equilibrium points, propagates reproducible particle clouds near L1 and L4, validates Jacobi-constant conservation, and compares how the ensembles spread over finite time.
02 / Motivation
The problem
The Earth-Moon CR3BP provides a useful bridge from classical mechanics to the dynamical structures that shape cislunar trajectory design.
03 / Method
Technical approach
The implementation uses Brent root finding for the collinear points, closed-form triangular points, high-accuracy solve_ivp integration, seeded Monte Carlo perturbations, and regression of ensemble RMS spread. The analysis explicitly distinguishes its finite-time L1 growth fit from a rigorous Lyapunov exponent.
04 / Reflection
What I learned
The work made numerical conservation checks, nondimensionalization, stability language, and the limits of finite-time regression much more concrete.