Challenge to anomalous phenomena in solar neutrino

Abstract

We suggest a would-be solution to the solar neutrino tension why solar neutrinos appear to mix differently from reactor antineutrinos, in theoretical respect. To do that, based on an extended theory with light sterile neutrinos added we derive a general transition probability of neutrinos born with one flavor tuning into a different flavor. Three new mass-squared differences are augmented in the extended theory: $$ \Delta {m}_{\mathrm{ABL}}^2\lesssim \mathcal{O}\left({10}^{-11}\right) $$ Δ m ABL 2 ≲ O 10 − 11 eV2 optimized at astronomical-scale baseline (ABL) oscillation experiments and one $$ \Delta {m}_{\mathrm{SBL}}^2\lesssim \mathcal{O}(1) $$ Δ m SBL 2 ≲ O 1 eV2 optimized at reactor short-baseline (SBL) oscillation experiments. With a so-called composite matter effect that causes a neutrino flavor change via the effects of sinusoidal oscillation including the Mikheyev-Smirnov-Wolfenstein matter effect, we find that the value of ∆m2 measured from reactor antineutrino experiments can be fitted with that from the 8B solar neutrino experiments for roughly $$ \Delta {m}_1^2\lesssim {10}^{-13} $$ Δ m 1 2 ≲ 10 − 13 eV2 and $$ \Delta {m}_2^2\simeq \mathcal{O}\left({10}^{-11}\right) $$ Δ m 2 2 ≃ O 10 − 11 eV2. Nonetheless, we find that the current data (solar neutrino alone) is not precise enough to test the proposed scenario. Future precise measurements of 8B and pep solar neutrinos may confirm and/or improve the value of $$ \Delta {m}_2^2 $$ Δ m 2 2 .