Abstract
The phenomenon of tidal evolution in the motion of planets in the solar system is studied using the many-parameter model of the linear theory of viscoelasticity. The planet is modelled as an almost spherical viscoelastic body whose centre of mass moves in an elliptical orbit. The method of averaging is used to obtain the equations describing the evolution of plane rotational motion in the non-resonant and resonant cases. The limiting angular velocity and conditions for the existence of a stable resonant rotation are obtained as functions of the eccentricity and of the parameters characterizing the properties of the material of the planet. The ranges of variation of these parameters for which the results agree with those obtained earlier on the basis of the hypotheses concerning the structure of the momentum of tidal forces /1, 2/, or by using the Kelvin-Voigt model for the planet material and introducing additional assumptions about its properties /3, 4/ are indicated.
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