Open AccessOn the source regions for mare picrite glasses
Author(s) -
Hess Paul C.
Publication year - 2000
Publication title -
journal of geophysical research: planets
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/1999je001067
Subject(s) - geology , basalt , fractional crystallization (geology) , anorthosite , geochemistry , magma , olivine , crust , geology of the moon , ilmenite , lunar mare , petrology , plagioclase , volcano , paleontology , quartz
Models for the crystallization of the magma ocean, phase equilibria constraints, and geochemical criteria constrain the mare basalt source region to lie deep within the Moon and within olivine‐orthopyroxene cumulate layers of the magma ocean. The Mg* compositions of the mare basalt source region, the ferroan anorthosite crust and the mg‐suite troctolites, require that most if not all the cumulates were produced by a magma ocean undergoing fractional rather than equilibrium crystallization. Estimates of the depth of the elastic lithosphere, the existence of mascons, and the need to sequester some heat‐producing elements in the lunar interior are consistent with the lunar overturn model which transports the refractory cumulates, the more fertile ilmenite‐diopside cumulates and some of the KREEP components into the lunar interior.