The Mikheyev-Smirnov-Wolfenstein model of resonant solar-neutrino oscillations is discussed for three generations of leptons. Assuming adiabatic transitions, bounds for the and e-neutrinos mass-squared difference 21,0 are obtained as a function of the mixing angle theta1. The allowed region in the 21,0-theta1 plot that would solve the solar-neutrino problem is shown to be substantially larger than that of the two-generation case. In particular, the difference between the two- and three-generation cases becomes significant for theta1 larger than 20°.
ASJC Scopus subject areas