The Solution of the Solar Neutrino Problem

Details The Solution of the Solar Neutrino Problem The Solution of the Solar Neutrino Problem

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dnp.ba001b&link_type=abstract

American Physical Society, 2002 Fall Meeting of the Division of Nuclear , abstract #BA.001

Physics

Scientific paper

The decades-old solar neutrino problem can be simply stated: that the measured flux of electron neutrinos is only about one-third as large as predicted by theory. Recent results from the Sudbury Neutrino Observatory (SNO) have for the first time clearly shown that the missing two-thirds of the predicted flux arrives at the detectors as mu and tau neutrinos. This is a spectacular success, and is very strong evidence for neutrino mass and mixing, in particular the large-mixing-angle (LMA) solution. These results have far-reaching implications, from the solar core temperature to models of neutrino mass to the lepton number of the universe. I will also discuss the key role of ongoing nuclear-physics efforts to reduce the uncertainties on the predicted neutrino fluxes and detection cross sections. Though one important aspect of the solar neutrino problem has been "solved", the upcoming low-energy solar neutrino experiments and the KamLAND reactor antineutrino experiment will play a very important role in exploring the rest of the story.

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