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.

References:

BELLINI 2012A PRL 108 051302 First Evidence of ${{\mathit p}}{{\mathit e}}{{\mathit p}}$ Solar Neutrinos by Direct Detection in Borexino