Contribution of tidal dissipation to lunar thermal history. Evidence for lunar true polar wander and a past low-eccentricity, synchronous lunar orbit. Evidence for a past high-eccentricity lunar orbit. Formation of terrestrial planets from protoplanets under a realistic accretion condition. Tidal friction in the Earth–Moon system and Laplace planes: Darwin redux. Obliquity evolution of extrasolar terrestrial planets. Dynamical instabilities in high-obliquity systems. Secular perturbations of asteroids with high inclination and eccentricity. Satellite dynamics on the Laplace surface. in Irregular Satellites of the Giant Planets 411–424 (Univ. Strong ocean tidal flow and heating on moons of the outer planets. Tidal dissipation in the early lunar magma ocean and its effect on the evolution of the Earth–Moon system. Tidal evolution in the Neptune–Triton system. Early evolution of the Earth–Moon system with a fast-spinning Earth. New approaches to the Moon’s isotopic crisis. Equilibration in the aftermath of the lunar-forming giant impact. Origin of the Moon in a giant impact near the end of the Earth’s formation. Satellite-sized planetesimals and lunar origin. A new model for lunar origin: equilibration with Earth beyond the hot spin stability limit. Forming a Moon with an Earth-like composition via a giant impact. Making the Moon from a fast-spinning Earth: a giant impact followed by resonant despinning. Oxygen isotopic evidence for vigorous mixing during the Moon-forming giant impact. Isotopic Composition of the Moon and the Lunar Isotopic Crisis 1–13 (Springer, 2015) Collisionless encounters and the origin of the lunar inclination. Origin of the Moon’s orbital inclination from resonant disk interactions. Resonances in the early evolution of the Earth–Moon system. Our tidal evolution model supports recent high-angular-momentum, giant-impact scenarios to explain the Moon’s isotopic composition 6, 7, 8 and provides a new pathway to reach Earth’s climatically favourable low obliquity. Using numerical modelling, we show that the solar perturbations on the Moon’s orbit naturally induce a large lunar inclination and remove angular momentum from the Earth–Moon system. We present a tidal evolution model starting with the Moon in an equatorial orbit around an initially fast-spinning, high-obliquity Earth, which is a probable outcome of giant impacts. Here we show that tidal dissipation due to lunar obliquity was an important effect during the Moon’s tidal evolution, and the lunar inclination in the past must have been very large, defying theoretical explanations. In addition, the giant-impact theory has been challenged by the Moon’s unexpectedly Earth-like isotopic composition 4, 5. In the giant-impact hypothesis for lunar origin, the Moon accreted from an equatorial circum-terrestrial disk however, the current lunar orbital inclination of five degrees requires a subsequent dynamical process that is still unclear 1, 2, 3.
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