Boron neutrino flux and the MSW solution of the solar neutrino problem

摘要

There are large uncertainties in the predictions of the boron neutrino flux from the Sun which cannot be considered as being of purely statistical origin. We treat the magnitude of this flux, (Phi)(sub B), as a parameter to be found from experiment. The properties of the, MSW solution to the solar neutrino problem for different values of (Phi)(sub B) are studied. Present, data give the bounds: 0.38 < (Phi)(sub B)/(Phi)(sub B)(sup O) < 3.1 (2(sigma)), where (Phi)(sub B)(sup O) (identical to) 5.7 (center dot) 10(sup 6) cm(sup (minus)2)s(sup (minus)1) is the flux in the reference SSM. The variations of the flux in this interval enlarge the allowed region of mixing angles: sin(sup 2) 2(theta) = 0.2 (divided by) 2 (center dot) 10(sup (minus)4) (divided by) 2 (center dot) 10(sup (minus)2) (small mixing solutions) and sin(sup 2) 2(theta) = 0.2 (divided by) 0.85 (large mixing solution). If the value of the original boron neutrino flux is about that measured by Kamiokande, a consistent description of the data is achieved for sin(sup 2) 2(theta) (approximately) (0.8 (divided by) 2) (center dot) 10(sup (minus)3) (''very small mixing solution''). The solution is characterized by a strong suppression of the beryllium neutrino line, a weak distortion of the high energy part of the baron neutrino spectrum and a value of the double ratio (CC/NC)(sup exp)/(CC/NC)(sup SSM) at E > 5 MeV close to 1. We comment on the possibility to measure the neutrino parameters and the original boron neutrino flux in future experiments.