In-ice radio detection of GZK neutrinos

Models for the source and propagation of cosmic rays are stressed by observations of cosmic rays with energies E>1020 eV. A key discriminant between different models may be complementary observations of neutrinos with energies E>1018 eV. Independent of the source of the cosmic rays, neutrinos are produced during propagation via the GZK mechanism. Event rates for GZK neutrinos are expected to be in the range of 0.01-0.1 per km3 yr, suggesting a detector mass in excess of 1 Eg. Detection of radio cherenkov emission from showers produced in Antarctic ice may be an economical way to instrument such a large mass. It is suggested that a 100 km2 array of antennas centered on Icecube may allow confirmation of the radio technique and also increase the science achievable with Icecube by providing vertex information for events with thoroughgoing muons