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 2012 A 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.

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