Electron-Neutrino Majorana Mass and Solar Neutrino Oscillations

TL;DR

This paper explores the implications of Majorana neutrino masses on solar neutrino oscillations, deriving constraints on neutrino mass values based on radiative splitting calculations within a specific theoretical framework.

Contribution

It introduces a model linking Majorana masses of electron neutrinos and a linear combination of mu and tau neutrinos, deriving radiative splitting formulas applicable to solar neutrino oscillation solutions.

Findings

Neutrino mass constrained between 0.20 and 0.36 eV for given parameters.

Radiative splitting formula applicable to small-angle matter-enhanced oscillations.

Model restricts neutrino mass scale based on heavy scalar triplet interactions.

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.