Geochemical mapping of the Moon by orbital gamma-ray spectroscopy

Chemical compositions of the surfaces of the moon and certain planetary bodies can be determined by orbital γ-ray spectroscopy. The major sources of γ-ray lines (and of radionuclides) in the moon are the decay of the primordial radioelements (U, Th, and 40K) and nuclear reactions induced by the bombardment of the moon by cosmic-ray particles. The major cosmogenic γ-ray lines are produced by neutron nonelastic scattering and neutron capture reactions. The fluxes of γ-ray lines expected from the moon for each major source have been calculated. Gamma-rays from the moon were measured by γ-ray spectrometers during the Apollo 15 and 16 missions. The preliminary analysis of the data show that 0 and Si vary little over the moon's surface, that Mg, Fe, and Ti have higher concentrations in the maria than in the lunar highlands, and that the radioelements are significantly more abundant in and near the western nearside maria than in the rest of the moon. 2 figures, 5 tables