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- W3136200935 abstract "A bstract 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: $$ Delta {m}_{mathrm{ABL}}^2lesssim mathcal{O}left({10}^{-11}right) $$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML><mml:mi>Δ</mml:mi><mml:msubsup><mml:mi>m</mml:mi><mml:mi>ABL</mml:mi><mml:mn>2</mml:mn></mml:msubsup><mml:mo>≲</mml:mo><mml:mi>O</mml:mi><mml:mfenced><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>−</mml:mo><mml:mn>11</mml:mn></mml:mrow></mml:msup></mml:mfenced></mml:math> eV 2 optimized at astronomical-scale baseline (ABL) oscillation experiments and one $$ Delta {m}_{mathrm{SBL}}^2lesssim mathcal{O}(1) $$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML><mml:mi>Δ</mml:mi><mml:msubsup><mml:mi>m</mml:mi><mml:mi>SBL</mml:mi><mml:mn>2</mml:mn></mml:msubsup><mml:mo>≲</mml:mo><mml:mi>O</mml:mi><mml:mfenced><mml:mn>1</mml:mn></mml:mfenced></mml:math> eV 2 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 ∆ m 2 measured from reactor antineutrino experiments can be fitted with that from the 8 B solar neutrino experiments for roughly $$ Delta {m}_1^2lesssim {10}^{-13} $$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML><mml:mi>Δ</mml:mi><mml:msubsup><mml:mi>m</mml:mi><mml:mn>1</mml:mn><mml:mn>2</mml:mn></mml:msubsup><mml:mo>≲</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>−</mml:mo><mml:mn>13</mml:mn></mml:mrow></mml:msup></mml:math> eV 2 and $$ Delta {m}_2^2simeq mathcal{O}left({10}^{-11}right) $$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML><mml:mi>Δ</mml:mi><mml:msubsup><mml:mi>m</mml:mi><mml:mn>2</mml:mn><mml:mn>2</mml:mn></mml:msubsup><mml:mo>≃</mml:mo><mml:mi>O</mml:mi><mml:mfenced><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>−</mml:mo><mml:mn>11</mml:mn></mml:mrow></mml:msup></mml:mfenced></mml:math> eV 2 . Nonetheless, we find that the current data (solar neutrino alone) is not precise enough to test the proposed scenario. Future precise measurements of 8 B and pep solar neutrinos may confirm and/or improve the value of $$ Delta {m}_2^2 $$ <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML><mml:mi>Δ</mml:mi><mml:msubsup><mml:mi>m</mml:mi><mml:mn>2</mml:mn><mml:mn>2</mml:mn></mml:msubsup></mml:math> ." @default.
- W3136200935 created "2021-03-29" @default.
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- W3136200935 date "2021-03-01" @default.
- W3136200935 modified "2023-09-23" @default.
- W3136200935 title "Challenge to anomalous phenomena in solar neutrino" @default.
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- W3136200935 doi "https://doi.org/10.1007/jhep03(2021)115" @default.
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