Equilibrium points in the full three-body problem

The orbital motion of a spacecraft in the vicinity of a binary asteroid system can be modelled as the full three-body problem. The circular restricted case is considered here. Taking into account the shape, size, and mass distribution of arbitrarily shaped primary bodies, the locations of the equilibrium points are computed and are found to be offset from those of the classical CR3BP with point-masses. Through numerical computations, it was found that in cases with highly aspherical primaries, additional collinear and noncollinear equilibrium points exist. Examples include systems with pear-shaped and peanut-shaped bodies.