A Second Lunar Magma Ocean?
M ARION G RANGE * AND A LEXANDER N EMCHIN .
Curtin University, Department of Applied Geology, GPO box U1987, WA 6845, Perth, Australia.
*(correspondence:
m.grange@curtin.edu.au)
The Lunar Magma Ocean (LMO) model is one of the key concepts in the current understanding of lunar evolution. It is used to explain a range of geological, mineralogical and chemical characteristics of the Moon, such as the presence of anorthositic crust, a reservoir enriched in incompatible elements and mare basalts.
The LMO model suggests that the lunar crust, made up of Ferroan-Anorthosite (FAN), formed by segregation and floatation of plagioclase from the magma ocean, after ~75% of the initial liquid has crystallised as mafic cumulates. After ~95% solidification, the remaining liquid is enriched in incompatible elements (e.g. K, REE, P, U, Th, Zr
) and constitutes the KREEP reservoir. Although this reservoir has never been sampled as such, its existence is indicated by incompatible elements enrichment in some plutonic rocks, which are interpreted to be emplaced into the FAN crust. These rocks are also enriched in Mg and are referred to as Mg-suite. The presence of a KREEP component in this suite and the associated enrichment in incompatible elements also results in a widespread crystallisation of zircon in these rocks.
Very specific sequence of crystallisation predicted by the LMO model demands particular timing relationships between FAN, KREEP reservoir and Mg-suite rocks. However, absolute dating of FAN and Mg-suite samples reveals a significant overlap in ages that is inconsistent with the LMO model. In particular, the contradiction is highlighted by the recently obtained precise ages of (i) the oldest lunar zircon at 4417 ± 6 Ma [1], which must represent the youngest possible limit for the formation of KREEP reservoir and (ii) a sample of FAN at 4360 ± 3 Ma [2], which suggests the oldest limit for the lunar crust crystallisation.
The only way to resolve the controversy posed by chronological data is to accept the possibility of a second magma ocean on the Moon at ~4360 Ma, resulting from a massive impact and probably restricted to the near site of the Moon.
[1] Nemchin et al. (2009) Nature Geosc. 2, 133-136. [2] Borg et al. (2011), Nature 477, 70-73..