  We present simulation results for the detection of ultra-high energy (UHE)
cosmic ray (CR) and neutrino interactions in the Moon by radio-telescopes. We
simulate the expected radio signal at Earth from such interactions, expanding
on previous work to include interactions in the sub-regolith layer for single
dish and multiple telescope systems. For previous experiments at Parkes,
Goldstone, and Kalyazin we recalculate the sensitivity to an isotropic flux of
UHE neutrinos. Our predicted sensitivity for future experiments using the
Australia Telescope Compact Array (ATCA) and the Australian SKA Pathfinder
(ASKAP) indicate these instruments will be able to detect the more optimistic
UHE neutrino flux predictions, while the Square Kilometre Array (SKA) will also
be sensitive to all bar one prediction of a diffuse `cosmogenic', or `GZK',
neutrino flux.
  Current uncertainties concerning the structure and roughness of the lunar
surface prevents an accurate calculation of the sensitivity of the lunar
Cherenkov technique for UHE cosmic ray astronomy at high frequencies. However,
below 200 MHz we find that the proposed SKA low-frequency aperture array should
be able to detect events above 56 EeV at a rate about 30 times that of the
current Pierre Auger Observatory. This would allow directional analysis of UHE
cosmic rays, and investigation of correlations with putative cosmic ray source
populations, to be conducted with very high statistics.
