Using Proton Radiation from the Moon to Probe Regolith Hydrogenation in the Upper 1-10 cm

Detection of proton radiation from the Moon offers a new observational method for mapping compositional variations over the lunar surface. Recently, it was discovered that the yield of high energy "albedo" proton radiation coming from the lunar regolith due to bombardment by galactic cosmic rays (GCRs) depends on latitude: the yield increases toward higher latitudes. This dependence was attributed to a surface layer of hydrogenated regolith near the poles. Here, an improved technique is developed to use the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) on the Lunar Reconnaissance Orbiter to detect proton radiation from the lunar horizon and from lunar nadir and to use this to investigate diurnal variation in near-surface hydrogenation. Based on measurements taken in 2015, CRaTER observes an average proton albedo rate with a higher yield of protons from the lunar horizon than from the nadir. Both the average proton radiation albedo rate and the excess of proton radiation from the lunar horizon agree well with simulations. The measurements provide further evidence for the existence of the lunar hydrogenation layer. Lastly, CRaTER finds a yield (defined by the proton albedo divided by the GCR input) that is higher on the morning terminator compared to the evening terminator. Based on the observational statistics, there is a significant likelihood that the AM terminator produces a higher yield in the proton radiation albedo than the PM terminator during the period studied. While this presents some possible evidence of an AM enhancement, the excess could also potentially be explained by variation in GCR heavy species (He and heavier species). While initial results of an improved technique for measuring the proton radiation albedo are promising, the observational dataset utilized by CRaTER must be expanded significantly to reduce uncertainties in the search for temporal evolution and the excess of proton radiation from the lunar horizon as we probe hydrogenation excess in the upper 1 - 10 cm lunar regolith.