Detecting UHE neutrinos (E>1018eV) with a large radio array

Details Detecting UHE neutrinos (E>1018eV) with a large radio array Detecting UHE neutrinos (E>1018eV) with a large radio array

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999icrc....2..471s&link_type=abstract

Proceedings of the 26th International Cosmic Ray Conference. August 17-25, 1999. Salt Lake City, Utah, USA. Under the auspices o

Physics

Scientific paper

A relatively cost-effective way to detect ultra high energy (UHE) cosmic neutrinos is with an array of radio antennas buried in Antarctic ice. The GZK process `guarantees' such neutrinos as a result of interactions of high energy cosmic rays with the cosmic microwave background. A suitable geometry for detecting this flux is a large volume (104 km3 ) instrumented for contained events (100's of events per yr). For E ˜ 1018 eV, downward moving neutrinos would interact within the detector volume with probability 1:7 10,3 E =1018eV0:36. Upward neutrinos are shadowed by the Earth. High energy muons produced in cosmic ray air showers are negligible. The radio ice Cherenkov technique may permit construction of such a detector at modest cost. By detecting Cherenkov pulses from electromagnetic and hadronic cascades in the ice, an array of radio antennas would be able to detect and possibly identify all flavors of neutrino.

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