2006/01/24 by Hiroshi Nunokawa, Stephen Parke, R. Zukanovich Funchal +1
Physics and Astronomy · #Dark Matter and Cosmic Phenomena #Energy (signal processing) #Kinetic energy #Mass fraction #Neutrino #Neutrino Physics Research #Neutrino oscillation #Nuclear physics #Particle physics #Particle physics theoretical and experimental studies #Physics #Quantum mechanics #Solar neutrino #Thermodynamics #astro-ph #hep-ex #hep-ph #nucl-ex
paper · pdf · doi:10.1103/physrevd.74.013006
published as Phys.Rev.D74:013006,2006 · 23 pages, 8 postscript figures, latex. Dedicated to the memory of John Bahcall who championed solar neutrinos for many lonely years
arxiv created 2006/01/24 · openalex publication_date 2006/07/24 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/08
We calculate the fraction of 8B solar neutrinos that arrive at the Earth as a \ensuremathν2 mass eigenstate as a function of the neutrino energy. Weighting this fraction with the 8B neutrino energy spectrum and the energy dependence of the cross section for the charged current interaction on deuteron with a threshold on the kinetic energy of the recoil electrons of 5.5 MeV, we find the integrated weighted fraction of \ensuremathν2's to be (91\ifmmode±\else\textpm\fi2)% at the 95% CL. This energy weighting procedure corresponds to the charged current response of the Sudbury Neutrino Observatory (SNO). We have used SNO's current best fit values for the solar mass squared difference and the mixing angle, obtained by combining the data from all solar neutrino experiments and the reactor data from KamLAND. The uncertainty on the \ensuremathν2 fraction comes primarily from the uncertainty on the solar \ensuremathδm2 rather than from the uncertainty on the solar mixing angle or the standard solar model. Similar results for the Super-Kamiokande experiment are also given. We extend this analysis to three neutrinos and discuss how to extract the modulus of the Maki-Nakagawa-Sakata mixing matrix element Ue2 as well as place a lower bound on the electron number density in the production region for 8B solar neutrinos.