• We present 3D evolution models of the Moon coupled to its early bombardment history. • Thermal anomalies induced by impacts on the Moon decay within 100–200 Myrs. • Ejecta deposits modify surface he
The postimpact KREEP material distribution. For our model, the global KREEP material was initially resided at the bottom of crust with a thickness of 20 km. The giant impact excavated the crustal, KRE
- We determine the size of impactors for 16 lunar far-side basins from models of isostatically compensated gravity data. - We use the elastic thickness of the lithosphere to account for isostatic rela
• We model the surface evolution for a pre-Nectarian lunar surface unit• Relative to their size, large craters are less destructive to the surrounding terrain than small simple craters• A simple scale
