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There are 2-flavor solutions that describe the data well. 6. The Large-Mixing-Angle (LMA) and the ' L O W solutions survive, with LMA being considerably more probable (Fig. 3). Krastev and Smirnov17 find the best overall fit is for the LMA solution (see Table 3) but that other solutions are possible. Vacuum solutions tend to have significant shape distortions, which would be further disfavored if shape information from SNO were to be folded in to the analysis. Day-night effects arise from matter regeneration in the varying path through the earth's core.
Lett. B476, 40 (2000). 39 9. Measurement of Standard Model Processes in e+e Collisions at y/a ~203-209 GeV, OPAL Physics Note PN469. ch/Opal/ 10. VENUS Collaboration, K. Yusa et al, Phys. Lett. B447, 167 (1999). 11. L3 Collaboration, Determination of "f/Z Interference in e+e~ Annihilation at LEP, CERN-EP/2000-084. 12. J. Mnich, Tests of the Standard Model, CERN-EP/99-143. 13. L3 Collaboration, M. Acciarri et al, Phys. Lett. B470, 268 (1999). 14. G. Altarelli, B. Mele, and M. Ruiz-Altaba, Z. Phys.
3 a below the ES result, indicating the presence in the solar neutrino flux of active flavors other than electron. 05JIo;8i 50 Table 3: Two-flavor neutrino oscillation fits to the solar neutrino data, showing the 5 most probable solutions and the Goodness of Fit (Krastev and Smirnov 1 7 ). The hep flux is constrained to the SSM value, 8 B is free. Shape information from SK 1 6 but not S N O 1 6 is used. F. 34 and one sees that the flux of non-electron flavors is about twice that of the electron flavor.