This study examines the perturbed photogravitational Circular Restricted Three-Body Problem (CR3BP) under the combined effects of radiation pressure, albedo, continued fractional perturbations, and a gravitational disc. For the Sun–Earth system with the asteroid belt and the Sun–Jupiter system with the Kuiper belt, we analyze how the modified potential influences equilibrium points, Zero-Velocity Curves (ZVCs), and stability. Numerical results show that as the continued fractional parameter (epsilon ) increases, new collinear ((L_1', L_2')) and non-collinear ((L_4', L_5')) points emerge, while disc mass and other perturbations merely shift their locations. The Jacobi constant decreases with increasing (epsilon ), enlarging the allowed motion regions. Stability analysis indicates that (L_1, L_3, L_4', L_5') are unstable, whereas (L_4, L_5) remain stable within certain ranges of the critical mass ratio (mu _c). The new point (L_1') can be stable for specific (epsilon ) values in both systems. Overall, continued fractional perturbations, disc effects, and surface properties reshape equilibrium configurations and modify classical stability boundaries, enriching celestial dynamics and space mission design.
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