E. D. Hallman

A Heavy Water Detector to Resolve the Solar Neutrino Problem

Abstract The observation of the following three reactions: νed→ppe; νxe→νxe; and νxd→νxpn (where νx is any left- handed neutrino) in a heavy water Cerenkov detector which is being designed, allows the solar 8B ve flux, spectrum and direction to be measured. In addition, the total solar 8 Bν c neutrino flux, direction and integral spectrum, independent of neutrino flavor, may be determined to provide several independent methods to resolve the solar neutrino problem.

The Sudbury D2O Neutrino Detector

The construction of a solar neutrino observatory in a nickel mine near Sudbury, Canada, has been proposed[1]. This proposal is both attractive and timely because of the temporary surplus of over 1000 Mg of D2O stockpiled for the Canadian-designed nuclear power reactors, of the large rock overburden at the INCO mine and of the scientific interest in the solar neutrino flux and neutrino oscillations. The primary objective of the experiment is to measure the incident electron neutrino (νe) spectrum above 5 MeV in real time with energy and directional resolution. It is also expected that the total neutrino (νx) flux above 2.2 MeV can be measured thereby providing important information concerning neutrino oscillations. The observatory will also be a sensitive instrument for measuring neutrinos produced by cosmic rays, solar flares and collapsing stars.