Possible tomography of the Sun’s magnetic field with solar neutrinos

Abstract

The data from solar neutrino experiments together with standard solar model predictions are used in order to derive the possible profile of the magnetic field inside the Sun, assuming the existence of a sizeable neutrino magnetic moment and the resonant spin flavor mechanism. The procedure is based on the relationship between resonance location and the energy-dependent neutrino suppression, so that a large neutrino suppression at a given energy is taken to be connected to a large magnetic field in a given region of the Sun. In this way it is found that the solar field must undergo a very sharp increase by a factor of at least 6--7 over a distance no longer than 7--10% of the solar radius, decreasing gradually towards the surface. The range in which this sharp increase occurs is likely to be the bottom of the convective zone. There are also indications in favor of the downward slope being stronger at the start and more moderate on approaching the solar surface. Typical ranges for the magnetic moment are from a few times ${10}^{\ensuremath{-}13}{\ensuremath{\mu}}_{B}$ to its laboratory upper bounds while the mass square difference between neutrino flavours is ${\ensuremath{\Delta}}^{2}{m}_{21}\ensuremath{\simeq}(0.6--1.9)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}8}{\mathrm{eV}}^{2}.$