Fig. 5

(a) Distributions of neutron fluxes in the lunar subsurface calculated by the proton scaling method and alpha particle interaction models. Note that all of the patterns of calculations overlap in the individual distributions of fast, epithermal, and thermal neutrons, respectively. (b) Comparisons of neutron fluxes calculated at 55 points from the lunar surface to the first 3 m by the alpha particle interaction models of JQMD and JAMQMD with that by the proton scaling method.