POSSIBLE TOMOGRAPHY OF THE SUNS MAGNETIC-FIELD WITH SOLAR NEUTRINOS

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 sizeabl e 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 s uppression at a given energy is taken to be connected to a large magne tic field in a given region of the Sun. In this way it is found that t he solar field must undergo a very sharp increase by a factor of at le ast 6-7 over a distance no longer than 7-10 % of the solar radius, dec reasing gradually towards the surface. The range in which this sharp i ncrease occurs is Likely to be the bottom of the convective zone. Ther e are also indications in favor of the downward slope being stronger a t the start and more moderate on approaching the solar surface. Typica l ranges for the magnetic moment are from a few times 10-(13)mu(B), to its laboratory upper bounds while the mass square difference between neutrino flavours is Delta(2)m(21)similar or equal to(0.6-1.9)x10(-8) eV(2).