Improved measurement of 
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 solar neutrinos with 
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Agostini, M.; Altenmüller, K.; Appel, S.; Atroshchenko, V.; Bagdasarian, Z.; Basilico, D.; Bellini, G.; Benziger, J.; Bick, D.; Bravo, D.; Caccianiga, B.; Calaprice, F.; Caminata, A.; Cavalcante, P.; Chepurnov, A.; D’Angelo, D.; Davini, S.; Derbin, A.; Giacinto, A. Di; Marcello, V. Di; Ding, Xuefeng; Lüdovico, A. Di; Noto, L. Di; Drachnev, I.; Formozov, A.; Franco, D.; Galbiati, C.; Gschwender, M.; Ghiano, C.; Giammarchi, M.; Goretti, A.; Gromov, M.; Guffanti, D.; Hagner, C.; Houdy, T.; Hungerford, E.; Ianni, Aldo; Ianni, Andrea; Jany, A.; Jeschke, D.; Kobychev, V.; Korga, G.; Kumaran, S.; Lachenmaier, T.; Laubenstein, M.; Litvinovich, E.; Lombardi, P.; Lomskaya, I.; Ludhová, L.; Lukyanchenko, G.; Lukyanchenko, L.; Machulin, I.; Marcocci, S.; Martýn, J.; Meroni, E.; Meyer, M.; Miramonti, L.; Misiaszek, M.; Muratova, V.; Neumair, B.; Nieslony, M.; Nugmanov, R.; Oberauer, L.; Orekhov, V.; Ortica, F.; Pallavicini, M.; Papp, L.; Penek, Ö.; Pietrofaccia, L.; Pilipenko, N.; Pocar, A.; Raikov, G.; Ranalli, M. T.; Ranucci, G.; Razeto, A.; Re, A.; Redchuk, M.; Romani, A.; Rossi, N.; Rottenanger, S.; Schönert, S.; Semenov, D.; Skorokhvatov, M.; Smirnov, O.; Sotnikov, A.; Suvorov, Y.; Tartaglia, R.; Testera, G.; Thurn, J.; Unzhakov, E.; Vishneva, A.; Vogelaar, R. B.; Feilitzsch, F. von; Wójcik, Marcin; Wurm, M.; Zavatarelli, S.; Zuber, Κ.; Zuzel, G.

doi:10.1103/physrevd.101.062001

Cited by 51 publications

(85 citation statements)

References 35 publications

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“…This projection is shown in Fig. 3 (bottom) with solar neutrino measurements from Borexino [19,22], KamLAND [24], and SNO [25].…”

Section: Electroweak and Oscillation Parametersmentioning

confidence: 97%

“…(bottom) The ν e survival probability versus neutrino energy under the high-Z SSM. Dots represent the solar measurements of pp (green), 7 Be (blue), pep (orange), and 8 B (red) from Borexino [19,22]. The upward (downward) triangle shows a measurement of 7 Be ( 8 B) from KamLAND (SNO) [24,25].…”

Section: Flux and Luminositymentioning

confidence: 99%

“…Most recently, Borexino reported the first direct observation of carbon, nitrogen and oxygen (CNO) neutrinos at 5σ [20]. Five experiments, Borexino [21,22], Super-K [23], KamLAND [24], SNO [25], and SNO+ [26], have measured the higher-energy 8 B flux. COHERENT made the first observation of CEvNS [27], but astrophysical neutrinos have yet to be detected in this way.…”

Section: Introductionmentioning

confidence: 99%

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Solar neutrino detection sensitivity in DARWIN via electron scattering

Aalbers¹,

Agostini²,

Maouloud³

et al. 2020

Eur. Phys. J. C

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We detail the sensitivity of the proposed liquid xenon DARWIN observatory to solar neutrinos via elastic electron scattering. We find that DARWIN will have the potential to measure the fluxes of five solar neutrino components: pp, $$^7$$ 7 Be, $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep. The precision of the $$^{13}$$ 13 N, $$^{15}$$ 15 O and pep components is hindered by the double-beta decay of $$^{136}$$ 136 Xe and, thus, would benefit from a depleted target. A high-statistics observation of pp neutrinos would allow us to infer the values of the electroweak mixing angle, $$\sin ^2\theta _w$$ sin 2 θ w , and the electron-type neutrino survival probability, $$P_{ee}$$ P ee , in the electron recoil energy region from a few keV up to 200 keV for the first time, with relative precision of 5% and 4%, respectively, with 10 live years of data and a 30 tonne fiducial volume. An observation of pp and $$^7$$ 7 Be neutrinos would constrain the neutrino-inferred solar luminosity down to 0.2%. A combination of all flux measurements would distinguish between the high- (GS98) and low-metallicity (AGS09) solar models with 2.1–2.5$$\sigma $$ σ significance, independent of external measurements from other experiments or a measurement of $$^8$$ 8 B neutrinos through coherent elastic neutrino-nucleus scattering in DARWIN. Finally, we demonstrate that with a depleted target DARWIN may be sensitive to the neutrino capture process of $$^{131}$$ 131 Xe.

show abstract

“…This projection is shown in Fig. 3 (bottom) with solar neutrino measurements from Borexino [19,22], KamLAND [24], and SNO [25].…”

Section: Electroweak and Oscillation Parametersmentioning

confidence: 97%

Section: Flux and Luminositymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Solar neutrino detection sensitivity in DARWIN via electron scattering

Aalbers¹,

Agostini²,

Maouloud³

et al. 2020

Eur. Phys. J. C

Self Cite

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show abstract

“…Despite the successful description of the properties of three known neutrino species through decades of experimentation, we are faced with a growing list of anomalous phenomena -experimentally unexpected results that conflict with the three active neutrino oscillation standard framework (3νSF [1]): (i) the so-called "short-baseline (SBL) anomalies" [2][3][4][5][6][7][8][9][10][11][12][13] (including MiniBooNE data [14]), anomalous results measured in several experiments at distance less than 1 km, and (ii) the so-called "solar neutrino tension" [15][16][17] (see also refs. [18][19][20]), a discrepancy between the oscillation parameter determined in solar neutrino experiments and the one measured in reactor neutrino oscillation experiments. Although the solar neutrino tension (below 2σ uncertainties) seems small, the discrepancy has been the long-standing tension in the neutrino physics of 3νSF [15][16][17].…”

Section: Introductionmentioning

confidence: 93%

Challenge to anomalous phenomena in solar neutrino

Ahn

2021

J. High Energ. Phys.

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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 .

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“…Borexino has succeeded in determining all major solar neutrino flux components already with its first dataset Phase 1 (2007-10): first direct detections of pp [1] (Phase 2 data used), pep [2], 7 Be [3], and lowest-threshold observation of 8 B[4] at 3 MeV, as well as the best available limit in the CNO solar ν flux [4]. More recently, high-precision determinations of the aforementioned solar neutrino fluxes have been attained using new techniques and enlarged statistics from the post-LS-purification phase: Phase 2 [5] [6]. Geoneutrinos have also been measured with high significance (5.9σ [7]) by Borexino, thanks to the extremely clean ν e channel.…”

Section: Introductionmentioning

confidence: 99%