What Do We (Not) Know Theoretically about Solar Neutrino Fluxes?

Solar model predictions of $^{8}\mathrm{B}$ and $p\mathrm{\text{\ensuremath{-}}}p$ neutrinos agree with the experimentally determined fluxes (including oscillations): $\ensuremath{\varphi}(pp{)}_{\mathrm{measured}}=(1.02\ifmmode\pm\else\textpm\fi{}00.02\ifmmode\pm\else\textpm\fi{}0.01)\ensuremath{\varphi}(pp{)}_{\mathrm{theory}}$ and $\ensuremath{\varphi}(^{8}\mathrm{B}{)}_{\mathrm{measured}}=(0.88\ifmmode\pm\else\textpm\fi{}0.04\ifmmode\pm\else\textpm\fi{}0.23)\ensuremath{\varphi}(^{8}\mathrm{B}{)}_{\mathrm{theory}}$, $1\ensuremath{\sigma}$ experimental and theoretical uncertainties, respectively. We use improved input data for nuclear fusion reactions, the equation of state, and the chemical composition of the Sun. The solar composition is the dominant uncertainty in calculating the $^{8}\mathrm{B}$ and CNO neutrino fluxes; the cross section for the $^{3}\mathrm{He}(^{4}\mathrm{He},\ensuremath{\gamma})^{7}\mathrm{Be}$ reaction is the most important uncertainty for the calculated $^{7}\mathrm{Be}$ neutrino flux.

Hali tarjima qilinmagan