The Charged Neutrino: a New Approach to the Solar Neutrino Problem

We have considered the effect of the reduction of the solar neutrino flux on earth due to the deflection of the charged neutrino by the magnetic field of the solar convective zone. The antisymmetry of this magnetic field about the plane of the solar equator induces the anisotropy of the solar neutrino flux thus creating the deficit of the neutrino flux on the earth. The deficit has been estimated in terms of solar and neutrino parameters and the condition of a 50 % deficit has been obtained: QνgradH ≥ 10 −18eG/cm where Qν is the neutrino electric charge, gradH is the gradient of the solar toroidal magnetic field, e is the electron charge. Some attractive experimental consequences of this scenario are qualitatively discussed. The discrepancy between the results of the solar neutrino experiments [1–4] and the predictions of the Standard Solar Models [5,6] is one of the most challenging issues of modern particle physics and astrophysics. Some of the plausible solutions to the solar neutrino problem are neutrino oscillations amplified by the MikheevSmirnovWolfenstein effect [7,8], neutrino decay [9], neutrino spin-precession [10] in the solar magnetic field and resonant spin-flavour conversion scenario [11] (assuming the twisting structure of the solar magnetic field in the convective zone has recently led to a more complicated variant of the last scenario [12]). However, all the solutions proposed so far rely on some hypothetical properties of the