Quasi-energy-independent solar neutrino transitions
Quasi-energy-independent solar neutrino transitions
Current solar, atmospheric, and reactor neutrino data still allow oscillation scenarios where the squared mass differences are all close to ${10}^{\ensuremath{-}3} {\mathrm{eV}}^{2},$ rather than being hierarchically separated. For solar neutrinos, this situation (realized in the upper part of the so-called large-mixing angle solution) implies adiabatic transitions which depend weakly on …