This work presents a unified analytical framework for the origin and stabilization of Earth’s axial tilt (~23.5°), based on angular momentum transfer during a giant impact and subsequent dynamical evolution. Unlike conventional approaches that treat obliquity as a direct consequence of impact geometry, this study considers the present-day obliquity as a primary constraint. Using observational data from the Earth–Moon system, we derive the relationship between perpendicular and axial angular momentum components required to reproduce the observed tilt. The results indicate that a realistic giant impact produces an initial high obliquity (~40°–50°), which subsequently evolves toward a stable configuration (~23.5°) through angular momentum redistribution, rapid planetary rotation, and interaction with a proto-lunar disk. Furthermore, the study proposes that deep mantle structures, particularly Large Low Shear Velocity Provinces (LLSVPs), may preserve a spatial memory of early impact geometry. Reconstruction of their position in a zero-obliquity reference frame suggests a shift toward equatorial regions, consistent with efficient angular momentum transfer. The model provides testable predictions using seismic tomography and offers an alternative interpretation consistent with existing giant impact simulations.
Kujtim gjoka Gjoka (Tue,) studied this question.