Stars as Laboratories for Fundamental Physics - MPP Theory Group

Solar Neutrinos 369
Fig. 10.13. Measured over expected spectrum of recoil electrons from solar
neutrinos at Kamiokande, arbitrarily normalized to unity at E ν = 9.5 MeV
(Suzuki 1995).
Fig. 10.14. Limit on a solar ν e flux relative to 8 B solar ν e ’s from the isotropic
background shown in Fig. 10.11. The data used for this result extend until
August 1992 (Suzuki 1993).
be used to constrain the ν e flux. At different energies a 90% CL upper
limit on the solar ν e flux relative to 8 B solar neutrinos is shown
in Fig. 10.14 according to Suzuki (1993). The best relative limit is
at E ν = 13 MeV where the ν e flux is less than 5.8% of 8 B solar ν e ’s
at 90% CL. If the cause of the isotropic background could be reliably
identified these upper limits could be improved accordingly.