2012/04/04 by Jagadish Singh, Aishetu Umar · 3 citations
Engineering · Physics and Astronomy · #Astrophysics #Celestial mechanics #Classical mechanics #Cosmology and Gravitation Theories #Degenerate energy levels #Eccentricity (behavior) #Elliptic orbit #Lagrangian point #Mass ratio #Mean motion #Motion (physics) #Oblate spheroid #Physics #Primary (astronomy) #Pulsars and Gravitational Waves Research #Quantum mechanics #Radiation pressure #Spacecraft Dynamics and Control #Three-body problem
paper · pdf · doi:10.1088/0004-6256/143/5/109
openalex publication_date 2012/04/04 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
This paper studies the motion of an infinitesimal mass around seven equilibrium points in the framework of the elliptic restricted three-body problem under the assumption that the primary of the system is a non-luminous, oblate spheroid and the secondary is luminous. A practical application of this case could be the study of the dynamical evolution of dust particles in orbits around a binary system with a dark degenerate primary and a secondary stellar companion. Conditional stability of the motion around the triangular points exists for 0 < μ < μ c , where μ is the mass ratio. The critical mass ratio value μ c depends on the combined effect of radiation pressure, oblateness, eccentricity, and the semimajor axis of the elliptic orbits; an increase in any of these parameters has destabilizing results on the orbits of the test particles. The overall effect is therefore that the size of the region of stability decreases when the value of these parameters increases. The collinear points and the out-of-plane equilibrium points are found to be unstable for any combination of the parameters considered here. Further, a numerical exploration computing the positions of the triangular points and the critical mass ratio of two binaries RX J0450.1–5856 and Nova Cen 1969 (Cen X-4) is given.