  The Moon exhibits striking geological asymmetries in elevation, crustal
thickness, and composition between its nearside and farside. Although several
scenarios have been proposed to explain these asymmetries, their origin remains
debated. Recent remote sensing observations suggest that (1) the crust on the
farside highlands consists of two layers: a primary anorthositic layer with
thickness of ~30-50 km and on top a more mafic-rich layer ~10 km thick; and (2)
the nearside exhibits a large area of low-Ca pyroxene that has been interpreted
to have an impact origin. These observations support the idea that the lunar
nearside-farside asymmetries may be the result of a giant impact. Here, using
quantitative numerical modeling, we test the hypothesis that a giant impact on
the early Moon can explain the striking differences in elevation, crustal
thickness, and composition between the nearside and farside of the Moon. We
find that a large impactor, impacting the current nearside with a low velocity,
can form a mega-basin and reproduce the characteristics of the crustal
asymmetry and structures comparable to those observed on the current Moon,
including the nearside lowlands and the farside's mafic-rich layer on top of a
primordial anorthositic crust. Our model shows that the excavated deep-seated
KREEP (potassium, rare-earth elements, and phosphorus) material, deposited
close to the basin rim, slumps back into the basin and covers the entire basin
floor; subsequent large impacts can transport the shallow KREEP material to the
surface, resulting in its observed distribution. In addition, our model
suggests that prior to the asymmetry-forming impact, the Moon may have had an
182W anomaly compared to the immediate post-giant impact Earth's mantle, as
predicted if the Moon was created through a giant collision with the
proto-Earth.
