Electron-Neutrino Majorana Mass and Solar Neutrino Oscillations

Abstract

Assuming the Majorana masses of $\nu_e$ and the linear combination $c \nu_\tau - s \nu_\mu$ to be equal from their couplings to a heavy scalar triplet $\xi$, I show that their radiative splitting is given by $\Delta m^2/m_\nu^2 = (3 c^2/4 \pi^2) (G_F/\sqrt 2) m_\tau^2 \ln (m_\xi^2/m_W^2)$. This is applicable to the small-angle matter-enhanced oscillation solution of the solar neutrino deficit and restricts $m_\nu$ to be between 0.20 and 0.36 eV if $c^2 = 0.7$ and $m_\xi = 10^{14}$ GeV.