Fig. 4: Schematic summary illustrating formation pathways of ferromagnetic minerals in CE6 lunar soils and their corresponding remanent magnetization acquisition mechanisms.

Formation pathways include fractional crystallization from lunar magma and cooling of basaltic lava flows; recrystallization via impact-induced melting, delivery and deposition of exogenous meteoritic iron-rich materials; formation of spherical nano- to micron-scale metallic iron grains through impacts; and space-weathering processes such as solar wind irradiation and vapor deposition. These diverse origins make ferromagnetic minerals exhibit distinct physical, chemical, and magnetic properties, enabling the acquisition of various remanent magnetization: thermal (TRM), chemical (CRM), shock (SRM), viscous (VRM), and depositional (DRM). The coexistence of these magnetizations in lunar materials provides essential constraints for interpreting lunar dynamo history, crustal magnetic anomalies, and surface weathering evolution. The SPA crustal-structure model is adopted from refs. ^50,73., while our framework for space-weathering processes follows ref. ¹⁴. The topographic map of the moon is modified from ref. ⁷⁴. (NASA\SVS\Ernest T. Wright).