The existence of new equilibrium points is established in the restricted three-body problem with equal prolate primaries. These are located on the Z-axis above and below the inner Eulerian equilibrium point L 1 and give rise to a new type of straight-line periodic oscillations, different from the well known Sitnikov motions. Using the stability properties of these oscillations, bifurcation points are found at which new types of families of 3D periodic orbits branch out of the Z-axis consisting of orbits located entirely above or below the orbital plane of the primaries. Several of the bifurcating families are continued numerically and typical member orbits are illustrated.
We consider the photogravitational restricted three-body problem with oblateness and study the Sitnikov motions. The family of straight line oscillations exists only in the case where the primaries are of equal masses as in the classical Sitnikov problem and have the same oblateness coefficients and radiation factors. A perturbation method based on Floquet theory is applied in order to study the stability of the motion and critical orbits are determined numerically at which families of three-dimensional periodic orbits of the same or double period bifurcate. Many of these families are computed.
The stability evolution of family f of the planar circular restricted three-body problem in the Earth-Moon case is explored numerically using the Poincar茅 surface of section. It is shown that third order resonances are the main cause of the reduction of the stability region of retrograde satellites. Several branches of family f are also computed and these are seen by the configuration of their family characteristics to roughly determine the stability region. Previous results on smaller mass ratios of primaries are thus extended to the Earth-Moon system.
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