hep solar-neutrino flux measured via ${{\mathit \nu}}{{\mathit e}}$ elastic scattering. This process is sensitive to all active neutrino flavors, but with reduced sensitivity to ${{\mathit \nu}_{{\mu}}}$ , ${{\mathit \nu}_{{\tau}}}$ due to the cross-section difference, $\sigma\mathrm {( {{\mathit \nu}} _{{{\mathit \mu}} , {{\mathit \tau}} } {{\mathit e}} )}$ $\sim{}0.16\sigma\mathrm {( {{\mathit \nu}_{{e}}} {{\mathit e}} )}$. If the hep solar-neutrino flux involves nonelectron flavor active neutrinos, their contribution to the flux is $\sim{}0.16$ times of ${{\mathit \nu}_{{e}}}$ .

VALUE ($ 10^{3} $ cm${}^{-2}$s${}^{-1}$) CL% DOCUMENT ID TECN • • We do not use the following data for averages, fits, limits, etc. • • $<73$ 90 1 HOSAKA 2006 SKAM 1  HOSAKA 2006 result is obtained from the recoil electron energy window of $18 - 21$ MeV, and updates FUKUDA 2001 result.

References:

HOSAKA 2006 PR D73 112001 Solar Neutrino Measurements in Super-Kamiokande-I