Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory

Aharmim, B.; Ahmed, S.; Anthony, A. E.; Barros, N.; Beier, E. W.; Bellerive, A.; Beltrán, B.; Bergevin, M.; Biller, S. D.; Boudjemline, K.; Boulay, M. G.; Cai, B.; Chan, Y. D.; Chauhan, D.; Chen, M.; Cleveland, B. T.; Cox, G. A.; Dai, Xiongxin; Deng, Hui; Detwiler, J. A.; DiMarco, M.; Doe, P. J.; Doucas, G.; Drouin, P.‐L.; 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.; Gagnon, N.; Goon, J. Tm.; Graham, K.; Guillian, E.; Habib, S.; Hahn, R. L.; Hallin, A. L.; Hallman, E. D.; Harvey, P. J.; Hazama, R.; Heintzelman, W. J.; Heise, J.; Helmer, R. L.; Hime, A.; Howard, C.; Huang, M.; Jagam, P.; Jamieson, B.; Jelley, N. A.; Jerkins, M.; Keeter, K. J.; Klein, J. R.; Kormos, L. L.; Kos, M.; Kraus, C.; Krauss, C. B.; Krüger, A.; 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; Miller, Michael L.; Monreal, B.; Monroe, J.; 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.; Rosten, R.; Schwendener, M. H.; Secrest, J. A.; Seibert, S.; Simard, O.; Simpson, John; Skensved, P.; Sonley, T. J.; Stonehill, L. C.; Tešić, G.; Tolich, N.; Tsui, T.; Berg, R. Van; VanDevender, B. A.; Virtue, C. J.; Tseung, H. Wan Chan; Wark, D.; Watson, Peter; Wendland, J.; West, N.; Wilkerson, J. F.; Wilson, J. R.; Wouters, J.M.; Wright, A.; Yeh, M.; Zhang, F.; Zuber, Κ.

doi:10.1103/physrevc.88.025501

Cited by 401 publications

(466 citation statements)

References 48 publications

Supporting

Mentioning

442

Contrasting

Unclassified

Order By: Relevance

“…• event rates of solar neutrino radiochemical experiments Chlorine [91], GALLEX/GNO [92], and SAGE [93], as well as time-and energy-dependent rates from the four phases in Super-Kamiokande [94][95][96][97], the three phases of SNO [98], and Borexino [99,100];…”

Section: )mentioning

confidence: 99%

A White Paper on keV sterile neutrino Dark Matter

Adhikari

Agostini

et al. 2017

J. Cosmol. Astropart. Phys.

Self Cite

380

316

View full text Add to dashboard Cite

Abstract. We present a comprehensive review of keV-scale sterile neutrino Dark Matter, collecting views and insights from all disciplines involved -cosmology, astrophysics, nuclear, and particle physics -in each case viewed from both theoretical and experimental/observational perspectives. After reviewing the role of active neutrinos in particle physics, astrophysics, and cosmology, we focus on sterile neutrinos in the context of the Dark Matter puzzle. Here, we first review the physics motivation for sterile neutrino Dark Matter, based on challenges and tensions in purely cold Dark Matter scenarios. We then round out the discussion by critically summarizing all known constraints on sterile neutrino Dark Matter arising from astrophysical observations, laboratory experiments, and theoretical considerations. In this context, we provide a balanced discourse on the possibly positive signal from X-ray observations. Another focus of the paper concerns the construction of particle physics models, aiming to explain how sterile neutrinos of keV-scale masses could arise in concrete settings beyond the Standard Model of elementary particle physics. The paper ends with an extensive review of current and future astrophysical and laboratory searches, highlighting new ideas and their experimental challenges, as well as future perspectives for the discovery of sterile neutrinos.

show abstract

Section: )mentioning

confidence: 99%

A White Paper on keV sterile neutrino Dark Matter

Adhikari

Agostini

et al. 2017

J. Cosmol. Astropart. Phys.

Self Cite

380

316

View full text Add to dashboard Cite

show abstract

“…Neutrino oscillation parameters are mostly constrained by solar neutrino experiments [40][41][42][43][44][45], the SuperKamiokande atmospheric neutrino data [37], and accelerator data from MINOS [46], T2K [47], and the NuMI Off-Axis ν e Appearance Experiment (NOνA) [48]. These imply the existence of two hierarchical mass-squared differences ∆m 2 21 and ∆m 2 32 and three nonzero mixing angles θ 13 , θ 12 , θ 23 .…”

Section: Neutrino Parameter Measurementsmentioning

confidence: 99%

Neutrino versus antineutrino oscillation parameters at DUNE and Hyper-Kamiokande experiments

Gouvêa

Kelly

2017

Phys. Rev. D

View full text Add to dashboard Cite

Testing, in a non-trivial, model-independent way, the hypothesis that the three-massive-neutrinos paradigm properly describes nature is among the main goals of the current and the next generation of neutrino oscillation experiments. In the coming decade, the DUNE and Hyper-Kamiokande experiments will be able to study the oscillation of both neutrinos and antineutrinos with unprecedented precision. We explore the ability of these experiments, and combinations of them, to determine whether the parameters that govern these oscillations are the same for neutrinos and antineutrinos, as prescribed by the CPT-theorem. We find that both DUNE and Hyper-Kamiokande will be sensitive to unexplored levels of leptonic CPT-violation. Assuming the parameters for neutrino and antineutrino oscillations are unrelated, we discuss the ability of these experiments to determine the neutrino and antineutrino mass-hierarchies, atmospheric-mixing octants, and CP-odd phases, three key milestones of the experimental neutrino physics program. Additionally, if the CPT-theorem is violated in nature in a way that is consistent with all present neutrino and antineutrino oscillation data, we find that DUNE and Hyper-Kamiokande have the potential to ultimately establish leptonic CPT-invariance violation.

show abstract

“…Neglecting θ 13 , the fraction of this mass eigenstate which is detected as electron neutrino is |s 12 | 2 , while the fraction |c 12 s 23 sin θ τ | 2 is undetectable sterile. Hence, high energy charged current electron neutrino detection from solar neutrino experiments and the solar neutral current flux [63] can be used to constrain θ τ when combined with either the KamLAND determination of θ 12 or with the theoretical calculation of the 8 B flux. Because the KamLAND experiment, while very constraining of ∆m 2 12 , is not as sensitive to U e2 , the theoretical calculation of the 8 B flux currently gives the best precision on this determination.…”

Section: Jhep04(2015)170mentioning

confidence: 99%

Constraints and consequences of reducing small scale structure via large dark matter-neutrino interactions

Bertoni

Ipek

McKeen

et al. 2015

J. High Energ. Phys.

106

View full text Add to dashboard Cite

Cold dark matter explains a wide range of data on cosmological scales. However, there has been a steady accumulation of evidence for discrepancies between simulations and observations at scales smaller than galaxy clusters. One promising way to affect structure formation on small scales is a relatively strong coupling of dark matter to neutrinos. We construct an experimentally viable, simple, renormalizable model with new interactions between neutrinos and dark matter and provide the first discussion of how these new dark matter-neutrino interactions affect neutrino phenomenology. We show that addressing the small scale structure problems requires asymmetric dark matter with a mass that is tens of MeV. Generating a sufficiently large dark matter-neutrino coupling requires a new heavy neutrino with a mass around 100 MeV. The heavy neutrino is mostly sterile but has a substantial τ neutrino component, while the three nearly massless neutrinos are partly sterile. This model can be tested by future astrophysical, particle physics, and neutrino oscillation data. Promising signatures of this model include alterations to the neutrino energy spectrum and flavor content observed from a future nearby supernova, anomalous matter effects in neutrino oscillations, and a component of the τ neutrino with mass around 100 MeV.

show abstract

Combined analysis of all three phases of solar neutrino data from the Sudbury Neutrino Observatory

Cited by 401 publications

References 48 publications

A White Paper on keV sterile neutrino Dark Matter

A White Paper on keV sterile neutrino Dark Matter

Neutrino versus antineutrino oscillation parameters at DUNE and Hyper-Kamiokande experiments

Constraints and consequences of reducing small scale structure via large dark matter-neutrino interactions

Contact Info

Product

Resources

About