This work presents an integrated conceptual framework describing the early dynamical evolution of the Earth–Moon system. The model combines tidal dissipation, angular momentum transfer, debris disk dynamics following the giant impact, and a possible early magnetospheric interaction phase between Earth and the Moon. Immediately after the giant impact that produced the Moon, the system likely consisted of a rapidly rotating proto-Earth surrounded by a debris disk. Material outside the Roche limit accreted to form the Moon. During this early phase, gravitational torques between the debris disk and the proto-Moon may have driven rapid outward orbital migration. As the debris disk dissipated, tidal interactions between Earth and the Moon became the dominant mechanism controlling orbital evolution. Tidal torque decreases strongly with distance, approximately proportional to 1/D⁶, implying that tidal dissipation was much stronger when the Moon orbited closer to Earth. The model also considers the possibility that the early Moon orbited within Earth’s magnetosphere during the initial stages of the system’s evolution. If Earth’s magnetic field was stronger in the early planetary epoch, magnetospheric coupling between Earth and the Moon may have influenced the magnetic environment recorded in lunar rocks. A simplified differential formulation is introduced to describe orbital expansion and angular momentum transfer between Earth’s rotation and the lunar orbit. The model incorporates several dissipation regimes representing different evolutionary stages of the Earth–Moon system. The framework proposed here highlights the importance of considering multiple interacting physical processes—disk dynamics, tidal dissipation, angular momentum redistribution, and magnetospheric interaction—in reconstructing the early history of the Earth–Moon system.
Kujtim Gjoka (Sat,) studied this question.