Model-dependent and independent implications of the first Sudbury Neutrino Observatory results

Details Model-dependent and independent implications of the first Sudbury Neutrino Observatory results Model-dependent and independent implications of the first Sudbury Neutrino Observatory results

2001-06-21

arxiv.org/abs/hep-ph/0106247v1

Phys.Rev.D64:093007,2001

Physics

High Energy Physics

High Energy Physics - Phenomenology

9 pages + 7 figures

Scientific paper

10.1103/PhysRevD.64.093007

We briefly discuss some implications of the first solar \nu results from the Sudbury Neutrino Observatory (SNO) experiment in the charged-current channel. We first show that the present SNO response function is very similar to the Super-Kamiokande (SK) one above 8.6 MeV in kinetic electron energy. On the basis of such equivalence we confirm, in a completely model-independent way, the SNO evidence for an active, non-electron neutrino component in the SK event sample, with a significance greater than 3 sigma. Then, by assuming no oscillations into sterile neutrinos, we combine the SK+SNO data to derive allowed regions for two free parameters: (i) the ratio f_B of the true B \nu flux from the Sun to the corresponding value predicted by the standard solar model (SSM), and (ii) the \nu_e survival probability , averaged over the common SK and SNO response function. We obtain the separate 3sigma ranges: f_B=1.03^{+0.50}_{-0.58} (in agreement with the SSM central value, f_B=1) and =0.34^{+0.61}_{-0.18} (in >3sigma disagreement with the standard electroweak model prediction, =1, with strong anticorrelation between the two parameters. Finally, by taking f_B and its uncertainties as predicted by the SSM, we perform an updated analysis of the $2\nu$ active neutrino oscillation parameters (\delta m^2,\tan^2\omega) including all the solar \nu data, as well as the spectral data from the CHOOZ reactor experiment. We find that only the solutions at \tan^2\omega~O(1) survive at the 3sigma level in the global fit, with a preference for the one at high \delta m^2---the so-called large mixing angle solution.

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