Abstract
The stability of planar resonant periodic rotations of a rigid body around its centre of mass in a central Newtonian field of forces is considered. The orbit of the centre of mass of the satellite is assumed to be an elliptical one, the body’s inertia ellipsoid is general. Resonant rotations examined mean that the body makes 3 turns around its centre of mass during 2 revolutions of the centre of mass on its orbit (Mercury-type resonance 3:2). For the set of eccentricity value e ε [0,0.25] typical for planets’ ones the regions of stability in the first approximation and regions of unstability are built in three-dimensional space of parameters (eccentricity and two inertial parameters).
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