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To understand the evolution of the Moon, we numerically modeled mantleconvection and magmatism in a two-dimensional polar rectangular mantle.Magmatism occurs as an upward permeable flow of magma generated bydecompression melting through the convecting matrix. The mantle is assumed tobe initially enriched in heat-producing elements (HPEs) and compositionallydense ilmenite-bearing cumulates (IBC) at its base. Here, we newly show thatmagma generation and migration play a crucial role in the calculated volcanicand radial expansion/contraction history. Magma is generated in the deep mantleby internal heating for the first several hundred million years. A large volumeof the generated magma ascends to the surface as partially molten fingers andplumes driven by melt-buoyancy to cause a volcanic activity and radialexpansion of the planet with the peak at 3.5-4 Gyr ago. Eventually, however,the planet begins to radially contract when the mantle solidifies by coolingfrom the surface boundary. As the mantle is cooled, the activity of partiallymolten plumes declines but continues for billions of years after the peakbecause some basal materials enriched in the dense IBC components hold HPEs.The calculated volcanic and radial expansion/contraction history is consistentwith the observed history of the Moon. Our simulations suggest a substantialfraction of the mantle was solid, and there was a basal layer enriched in HPEsand the IBC components at the beginning of the history of the Moon.

The volcanic and radial expansion/contraction history of the Moon simulated by numerical models of magmatism in the convective mantle