Introduction of tides in the spin-orbit problem

Abstract

The rotation of a non-spherical body (secondary) is disturbed by the torque of the main body (primary). One of the main objectives of the master's thesis of Filipe Batista Ribeiro (proc. 2012/21611-5) is to study the dynamics rotation of a Super-Earth with a conservative spin-orbit resonance model more general than the classical model (Goldreich & Peale 1966). While certain approaches are still held, such as the absence of obliquity of the rotation axis, our model includes planetary perturbations in the orbit of the planet whose rotation is being studied, and differentiated internal structure of the planet (Valencia et al . 2006). As discussed in Callegari & Rodríguez (2013), in the case of Hot Super-Earth with orbital periods of the order of days or less, tidal torques can dominate the perturbations in the planetary rotational motion. In fact, depending of parameters such as the coefficient of non-sphericity of the planet, planetary dissipation coefficient, etc., the stability of the spin-orbit resonance is not guaranteed (Goldreich 1966). The original project does not include among its objectives the inclusion of dissipative effects introduced by the tide. This BEPE project aims such goal, plus additional student education, aims to refine the results presented in Appendix 2 Callegari & Rodríguez (2013). (AU)