The restricted three-body problem including radiation pressure

Motion around the Triangular Equilibrium Points in the Circular Restricted Three-Body Problem under Triaxial Luminous Primaries with Poynting-Robertson Drag

“…The equation of motion was derived and despite the absence of the Jacobi integral there still exist six equilibrium points which were found to be unstable owing to the presence of PR-drag. In the investigation conducted by [10], the equilibrium points are seen to be unstable due to the destabilizing effect of PR-drag. [33] investigated the location and linear stability of the five Lagrangian points when the third body is acted upon by various drag forces, and these forces are seen to have destabilizing tendencies.…”

“…This circular restricted three-body problem (CR3BP) describes the motion of the infinitesimal mass moving in circular orbits and thus will not sufficiently describe the motion when certain perturbing forces are involved. This led scientists and mathematicians into an extensive study of the circular restricted three-body problem (CR3BP) from which models have been developed on the basis of different perturbing forces [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21].…”

“…This problem was first formulated by [31,32], and in 1937 Robertson modified Poynting's idea by basing his argument on Einstein's relativity theory from which he formulated a new radiation force. Subsequent examinations of the problem by researchers [23,10,33,34,35,25,26] have shown that P-R drag has a destabilizing effect on the stability of triangular equilibrium points. The authors of [23] modelled a problem in which the bigger primary is an intense emitter of radiation with [6] as the classical case.…”

The effect of radiation pressure on the equilibrium points in the generalized photogravitational restricted three body problem

“…It is acceptable to speak about a reduced mass of the particle as the effect of reducing its mass depends on the properties of the particle itself. Chernikov (1970) and Schuerman (1980) discussed the position as well as the stability of the Lagrangian equilibrium points when radiation pressure, P-R drag force are included. Murray (1994) systematically discussed the dynamical effect of general drag in the planar circular restricted three body problem.…”

Artificial equilibrium points for a generalized sail in the circular restricted three-body problem

“…In particular Perezhogin (1976); Kunitsyn and Perezhogin (1978); Schuerman (1980); Simmons et al (1985); Perezhogin and Tureshbaev (1989) investigated the effects of the thrust due to the radiation pressure on the CR3BP and showed that seven equilibrium points exist if one of the massive bodies is luminous. This problem is equivalent to consider a photonic (or solar) sail, whose thrust direction is fixed and radial with respect to the luminous body.…”