EQUILIBRIUM POINTS OF ELONGATED CELESTIAL BODIES AS THE PERTURBED ROTATING MASS DIPOLE
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abstract
The rotating mass dipole is adopted in this paper to approximate the gravitational field of the elongated celestial bodies. The equations of motion of the perturbed dipole model with oblateness of both primaries are derived to allow the existence of additional equilibrium points, including the points in the equatorial plane and in the plane xoz. Numerical simulations are performed to show the distribution of these equilibrium points along with zero-velocity curves around the dipole model. The effects of the oblateness of the primaries on the topological structure are also discussed based on the variation of zero-velocity curves.
