The paper investigates the evolution of translational-rotational motion of a double planet in the gravitational force field of a much heavier planet. It is assumed, that the distance between the center of mass of the attracting planet is much larger than the distance between the centers of mass of the two planets forming the double planet. All of the planets in the system are modeled as homogeneous isotropic bodies, occupying spherical regions in their non-deformed state. As an example, the double Earth-Moon in the Sun's gravitational force field is considered.
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