Measurement of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msub><mml:mi>ν</mml:mi><mml:mi>e</mml:mi></mml:msub></mml:math>and total<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mrow /><mml:mn>8</mml:mn></mml:msup></mml:math>B solar neutrino fluxes with the Sudbury Neutrino Observatory phase-III data set

Aharmim, B.; Ahmed, S.; Amsbaugh, J. F.; Anaya, Juan Manuel; Anthony, A. E.; Banar, J.; Barros, N.; Beier, E. W.; Bellerive, A.; Beltrán, B.; Bergevin, M.; Biller, S. D.; Boudjemline, K.; Boulay, M. G.; Bowles, T. J.; Browne, M. C.; Bullard, T. V.; Burritt, T. H.; Cai, B.; Chan, Y. D.; Chauhan, D.; Chen, M.; Cleveland, B. T.; Cox, G. A.; Currat, C.; Dai, Xiongxin; Deng, Hui; Detwiler, J. A.; DiMarco, M.; Doe, P. J.; Doucas, G.; Dragowsky, M. R.; Drouin, P.‐L.; Duba, C. A.; Duncan, F. A.; Dunford, M.; Earle, E.D.; Elliott, S. R.; Evans, H. C.; Ewan, G. T.; Farine, J.; Fergani, H.; Fleurot, F.; Ford, R.; Formaggio, J. A.; Fowler, Μ. M.; Gagnon, N.; Germani, J. V.; Goldschmidt, A.; Goon, J. Tm.; Graham, K.; Guillian, E.; Habib, S.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Hamian, A. A.; Harper, G.; Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Henning, R.; Hime, A.; Howard, C.; Howe, M. A.; Huang, M.; Jagam, P.; Jamieson, B.; Jelley, N. A.; Keeter, K. J.; Klein, J. R.; Kormos, L. L.; Kos, M.; Krüger, A.; Kraus, C.; Krauss, C. B.; Kutter, T.; Kyba, Christopher C. M.; Lange, R.; Law, J.; Lawson, I.; Lesko, K. T.; Leslie, J. R.; Loach, J. C.; MacLellan, R.; Majerus, Steve; Mak, H. B.; Maneira, J.; Martin, R. D.; McCauley, N.; McDonald, A.B.; McGee, Steven; Mifflin, C.; Miller, Guthrie; Miller, Michael L.; Monreal, B.; Monroe, J.; Morissette, B.; Myers, A.W.; Nickel, B. G.; Noble, A. J.; O’Keeffe, H. M.; Oblath, N. S.; Ollerhead, R. W.; Gann, G. D. Orebi; Oser, S. M.; Ott, R. A.; Peeters, S. J. M.; Poon, A. W. P.; Prior, G.; Reitzner, S. D.; Rielage, K.; Robertson, B.C.; Robertson, R. G. H.; Rollin, E.; Schwendener, M. H.; Secrest, J. A.; Seibert, S.; Simard, O.; Simpson, John; Skensved, P.; Smith, M. W. E.; Sonley, T. J.; Steiger, Thomas; Stonehill, L. C.; Tešić, G.; Thornewell, P. M.; Tolich, N.; Tsui, T.; Tunnell, C.; Wechel, T. Van; Berg, R. Van; VanDevender, B. A.; Virtue, C. J.; Wall, B. L.; Waller, D.; Tseung, H. Wan Chan; Wendland, J.; West, N.; Wilhelmy, J.B.; Wilkerson, J. F.; Wilson, J. R.; Wouters, J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, Κ.

doi:10.1103/physrevc.87.015502

Cited by 61 publications

(46 citation statements)

References 56 publications

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“…(ii) exploiting neutral current events, which are sensitive to any disappearance of active neutrinos. This approach allows us to derive constraints from the sterile neutrino searches in MINOS/MINOS+ [43] and NOνA [44], and from SNO solar neutrino data [79][80][81]. The corresponding analysis codes used in our fit are the same as discussed in sections III and V. Compared to ref.…”

Section: Constraints On |U τ 4 |mentioning

confidence: 99%

Updated global analysis of neutrino oscillations in the presence of eV-scale sterile neutrinos

Dentler

Hernández-Cabezudo

Kopp

et al. 2018

J. High Energ. Phys.

374

435

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We discuss the possibility to explain the anomalies in short-baseline neutrino oscillation experiments in terms of sterile neutrinos. We work in a 3 + 1 framework and pay special attention to recent new data from reactor experiments, IceCube and MINOS+. We find that results from the DANSS and NEOS reactor experiments support the sterile neutrino explanation of the reactor anomaly, based on an analysis that relies solely on the relative comparison of measured reactor spectra. Global data from the ν e disappearance channel favour sterile neutrino oscillations at the 3σ level with ∆m 2 41 ≈ 1.3 eV 2 and |U e4 | ≈ 0.1, even without any assumptions on predicted reactor fluxes. In contrast, the anomalies in the ν e appearance channel (dominated by LSND) are in strong tension with improved bounds on ν µ disappearance, mostly driven by MINOS+ and IceCube. Under the sterile neutrino oscillation hypothesis, the p-value for those data sets being consistent is less than 2.6 × 10 −6 . Therefore, an explanation of the LSND anomaly in terms of sterile neutrino oscillations in the 3 + 1 scenario is excluded at the 4.7σ level. This result is robust with respect to variations in the analysis and used data, in particular it depends neither on the theoretically predicted reactor neutrino fluxes, nor on constraints from any single experiment. Irrespective of the anomalies, we provide updated constraints on the allowed mixing strengths |U α4 | (α = e, µ, τ ) of active neutrinos with a fourth neutrino mass state in the eV range. a modentle@uni-mainz.de

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Section: Constraints On |U τ 4 |mentioning

confidence: 99%

Updated global analysis of neutrino oscillations in the presence of eV-scale sterile neutrinos

Dentler

Hernández-Cabezudo

Kopp

et al. 2018

J. High Energ. Phys.

374

435

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“…6. The process ν e + e − → ν e + e − Let us turn to consideration of the process of elastic scattering of solar neutrinos on electrons ν e e − → ν e e − , taking into account the conditions and the results of experiments at Super-Kamiokande [28]- [30] and at the Sudbury Neutrino Observatory (SNO) [31]- [34].…”

Section: Cross-sections and Kinematics Of The Elastic Neutrino-nucleomentioning

confidence: 99%

“…Noting good agreement between the results of our calculations and the results of experiments concerning the effective neutrino fluxes which correspond to the events of elastic νescattering and the reaction ν e D → e − pp, we draw attention to the fact that the difference between theoretical values of the effective fluxes describing the two processes is due to the change in the shape of the solar neutrino spectrum because of their collisions with the nucleons of the Sun and due to different dependence of the cross sections of processes on the neutrino energy. [34].…”

Section: Cross-sections and Kinematics Of The Elastic Neutrino-nucleomentioning

confidence: 99%

The Solar Neutrino Problem as Evidence of New Interaction

Slad

2019

J. Exp. Theor. Phys.

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A new concept is proposed to solve the solar neutrino problem, that is based on a hypothesis about the existence of a new interaction of electron neutrinos with nucleons mediated by massless pseudoscalar bosons. At every collision of a neutrino with nucleons of the Sun, its handedness changes from left to right and vice versa, and its energy decreases. The postulated hypothesis, having only one free parameter, provides a good agreement between the calculated and experimental characteristics of all five observed processes with solar neutrinos. * slad@theory.sinp.msu.ru

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“…Several experiments, like LSND, 1 SK, 2 SNO, 3 and MiniBooNE 4 among others, [5][6][7][8][9][10] have provided evidences of neutrino oscillations caused by non-zero neutrino masses. In particular, the results of LSND and MiniBooNE are compatible with the inclusion of at least an extra sterile neutrino.…”

Section: Introductionmentioning

confidence: 99%

Neutrino-induced reactions in core-collapse supernovae: Effects on the electron fraction

Saez

Civitarese

Mosquera

2018

Int. J. Mod. Phys. D

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Neutrino induced reactions are a basic ingredient in astrophysical processes like star evolution. The existence of neutrino oscillations affects the rate of nuclear electroweak decays which participates in the chain of events that determines the fate of the star. Among the processes of interest, the production of heavy elements in core-collapse supernovae is strongly dependent upon neutrino properties, like the mixing between different species of neutrinos.In this work we study the effects of neutrino oscillations upon the electron fraction as a function of the neutrino mixing parameters, for two schemes: the 1 + 1 scheme (one active neutrino and one sterile neutrino) and the 2 + 1 scheme (two active neutrinos and one sterile neutrino). We have performed this analysis considering a core-collapse supernovae and determined the physical conditions needed to activate the nuclear reaction chains involved in the r-process. We found that the interactions of the neutrinos with matter and among themselves and the initial amount of sterile neutrinos in the neutrinosphere might change the electron fraction, therefore affecting the onset of the r-process. We have set constrains on the active-sterile neutrino mixing parameters. They are the square-mass-difference ∆m 2 14 , the mixing angle sin 2 2θ 14 , and the hindrance factor ξs for the occupation of sterile neutrinos. The calculations have been performed for different values of Xα, which is the fraction of α-particles. For Xα = 0 the r-process is taking place if ∆m 2 14 ≥ 2 eV 2 , sin 2 2θ 14 < 0.8 and ξs < 0.5. For larger values of Xα the region of parameters is strongly reduced. The present results are compared to results available in the literature.

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Measurement of theνeand total8B solar neutrino fluxes with the Sudbury Neutrino Observatory phase-III data set

Cited by 61 publications

References 56 publications

Updated global analysis of neutrino oscillations in the presence of eV-scale sterile neutrinos

Updated global analysis of neutrino oscillations in the presence of eV-scale sterile neutrinos

The Solar Neutrino Problem as Evidence of New Interaction

Neutrino-induced reactions in core-collapse supernovae: Effects on the electron fraction

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