Tidal Evolution and Spin-Orbit Dynamics: The Critical Role of Rheology

Abstract

This study analyzes secular dynamics using averaged equations that detail tidal effects on the motion of two extended bodies in Keplerian orbits. It introduces formulas for energy dissipation within each body of a binary system. The equations, particularly in contexts like the Sun-Mercury system, can be delineated into a fast-slow system. A significant contribution of this work is the demonstration of the crucial role complex rheological models play in the capture by spin-orbit resonances. This is particularly evident in the notable enlargement of the basin of attraction for Mercury's current state when transitioning from a single characteristic time rheology to a dual characteristic time model, under the constraint that both models comply with the same estimate of the complex Love number at orbital frequency. The study also underscores the importance of Mercury's elastic rigidity on secular timescales.