Neutrino Conversions in Solar Random Magnetic Fields
arXiv:hep-ph/9809376 · doi:10.1016/S0550-3213(99)00352-1
Abstract
We consider the effect of a random magnetic field in the convective zone of the Sun superimposed to a regular magnetic field on resonant neutrino spin-flavour oscillations. We argue for the existence of a field of strongly chaotic nature at the bottom of the convective zone. In contrast to previous attempts we employ in addition a model motivated regular twisting magnetic field profile. In this scenario electron antineutrinos are produced through cascades like , The expected signals in the different experiments (SK,GALLEX-SAGE, Homestake) are obtained as a function of the level of noise, regular magnetic field and neutrino mixing parameters. Previous results obtained for small mixing and ad-hoc regular magnetic profiles are reobtained. We confirm the strong suppression for large part of the parameter space of the -flux for high energy boron neutrinos in agreement with present data of the SK experiment. We find that MSW regions ( eV, both small and large mixing solutions) are stable up to very large levels of noise (P=0.7-0.8) but they are acceptable from the point of view of antineutrino production only for moderate levels of it (). For strong noise and reasonable regular magnetic field, any parameter region is excluded. As a consequence, we are allowed to reverse the problem and to put limits on r.m.s field strength and transition magnetic moments by demanding a particle physics solution to the SNP under this scenario.
27 pags., 10 eps figs Minor biblio. mistakes have been corrected
References in corpus (4)
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