Advanced information on the Nobel Prize in Physics 2002, 8 October 2002 Information Department, P.O. Box 50005, SE-104 05 Stockholm, Sweden Phone: +46 8 673 95 00, Fax: +46 8 15 56 70, E-mail:
[email protected], Website: www.kva.se Neutrino astronomy Two kinds of extraterrestrial neutrinos, solar neutrinos and supernovae neutrinos, have been observed and their measured fuxes, as well as energy spectra, shed a new light on astrophysics and particle physics. Neutrinos – unlike photons – are not required to have zero mass. Small but non-zero neutrino masses have major consequences for physics and astrophysics. Neutrinos are highly abundant in the universe and so even small neutrino masses can make signifcant contributions to the mass density of the universe. Non-zero neutrino masses requires new phy- sics meaning that the Standard Model for elementary particles must be modifed. Davis’ radiochemical experiment The neutrino was postulated in 1930 by Pauli to explain the continuous energy spectrum of electrons emitted in nuclear β decay. Fermi’s theory for weak interactions was developed during the 1930’s. At the time, neutrino interaction cross-sections were considered too small for neutrino detection. However, the large neutrino fuxes that later became available with nuclear reactors opened the feld of neutrino physics. The experimental confrmation of the neutrino came in an experiment in 1955 by Cowan and Reines. Pontecorvo and Alvarez (Pontecorvo 1946, Alvarez 1949) suggested reactor experiments using the reaction ν + 37Cl → 37Ar + e- to detect the neutrino. At the time there was no clear distinction bet- ween neutrino and antineutrino.