(A) Neutrino fluxes and event ratios

$\phi _{\boldsymbol ES}$ (CNO) INSPIRE search

CNO solar-neutrino flux measured via ${{\mathit \nu}_{{e}}}$ 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, $\sigma ({{\mathit \nu}}_{{{\mathit \mu}},{{\mathit \tau}}}{{\mathit e}}$) $\sim{}$ 0.2 ${\mathit \sigma (}$ ${{\mathit \nu}_{{e}}}{{\mathit e}}{)}$. If the CNO solar-neutrino flux involves non-electron flavor active neutrinos, their contribution to the flux is $\sim{}$ 0.2 times that of ${{\mathit \nu}_{{e}}}$.
VALUE ($ 10^{8} $ cm${}^{-2}$s${}^{-1}$) CL% DOCUMENT ID TECN  COMMENT
• • • We do not use the following data for averages, fits, limits, etc. • • •
$<7.7$ 90 1
BELLINI
2012A
BORX MSW-LMA solution assumed
1  BELLINI 2012A reports an upper limit of the CNO solar neutrino flux measured via ${{\mathit \nu}_{{e}}}$ elastic scattering. The data were collected between January 13, 2008 and May 9, 2010, corresponding to 20,409 ton$\cdot{}$day fiducial exposure.
  References:
BELLINI 2012A
PRL 108 051302 First Evidence of ${{\mathit p}}{{\mathit e}}{{\mathit p}}$ Solar Neutrinos by Direct Detection in Borexino