#### $\phi _{\mathit ES}$ (hep)

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
 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