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Athanassopoulos, C.; Auerbach, L. B.; Bauer, D.; Bolton, R. D.; Boyd, Britta; Burman, R. L.; Caldwell, D. O.; Cohen, I.; Dieterle, B.; Donahue, J. B.; Eisner, A. M.; Fazely, A. R.; Federspiel, F.J.; Garvey, G. T.; Gray, Mark Girard; Gunasingha, R. M.; Highland, V. L.; Imlay, R.; Johnston, K.; Louis, W. C.; Lu, A.; Margulies, J.; McIlhany, K.; Metcalf, W.; Reeder, R. A.; Sandberg, V.; Schillaci, M. E.; Smith, D.; Stancu, I.; Strossman, W.; Sullivan, M. K.; VanDalen, G. J.; Vernon, W.; Yx, Wang; White, D. H.; Whitehouse, D.; Works, D.; Xiao, Y. J.; Yellin, S.

doi:10.1103/physrevlett.75.2650

Cited by 512 publications

(271 citation statements)

References 12 publications

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“…Thus, in the limit ∆m 2 21 , ∆m 2 31 → 0 neutrino flavour transitions take place only between ν e , ν µ and ν s . 1 The corresponding 3-flavour evolution equation is…”

Section: Jhep08(2016)153mentioning

confidence: 99%

See 1 more Smart Citation

Atmospheric neutrinos, ν e-ν s oscillations and a novel neutrino evolution equation

Akhmedov

2016

J. High Energ. Phys.

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If a sterile neutrino ν s with an eV-scale mass and a sizeable mixing to the electron neutrino exists, as indicated by the reactor and gallium neutrino anomalies, a strong resonance enhancement of ν e -ν s oscillations of atmospheric neutrinos should occur in the TeV energy range. At these energies neutrino flavour transitions in the 3+1 scheme depend on just one neutrino mass squared difference and are fully described within a 3-flavour oscillation framework. We demonstrate that the flavour transitions of atmospheric ν e can actually be very accurately described in a 2-flavour framework, with neutrino flavour evolution governed by an inhomogeneous Schrödinger-like equation. Evolution equations of this type have not been previously considered in the theory of neutrino oscillations.

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“…Thus, in the limit ∆m 2 21 , ∆m 2 31 → 0 neutrino flavour transitions take place only between ν e , ν µ and ν s . 1 The corresponding 3-flavour evolution equation is…”

Section: Jhep08(2016)153mentioning

confidence: 99%

“…A number of anomalies observed in short baseline neutrino experiments can be explained through the existence of a sterile neutrino ν s with mass in the eV range [1][2][3][4][5][6][7][8][9][10][11][12] (see refs. [13][14][15][16][17] for reviews).…”

Section: Introductionmentioning

confidence: 99%

Atmospheric neutrinos, ν e-ν s oscillations and a novel neutrino evolution equation

Akhmedov

2016

J. High Energ. Phys.

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“…The scenario with an additional fourth (or more) light sterile neutrino was suggested in 1990s, after the report of anomalous event excess in the ν µ → ν e appearance [1,2] known as the LSND anomaly. In addition, GALLEX and SAGE experiments [3,4] reported ∼ 23% deficit in measured activity of the 51 Cr neutrino source inside 71 Ga-filled tanks.…”

Section: The Stereo Experimentsmentioning

confidence: 99%

Detector energy calibration in the STEREO neutrino experiment

Sergeyeva¹

2018

Proceedings of the European Physical Society Conference on High Energy Physics — PoS(EPS-HEP2017)

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The STEREO experiment was developed to investigate the hypothesis of a light sterile neutrino arising from the observed discrepancy between measured reactor antineutrino fluxes and revised flux predictions, known as the Reactor Antineutrino Anomaly. The detector is located at 10 m from the compact nuclear reactor core of the Institut LaueLangevin. The segmentation of the detector target in 6 cells allows measuring the neutrino energy spectrum at different baselines. Antineutrino interactions are detected by the inverse β -decay reaction in Gd-loaded liquid scintillator. STEREO started taking data in November 2016. About 70 days of data have been recorded during reactor operation and ∼ 25 days during reactor shut down. STEREO plans to record ∼ 150 days more in 2018. To perform a correct energy reconstruction of neutrino events, the detector energy response must be determined accurately. Different radioactive gamma-ray sources, from 0.5 to ≈ 4.4 MeV, are used to constrain the non-linearity of the scintillator response. Calibration data analysis provides the relation between the charge detected by the photomultipliers and the true deposited gamma energy obtained by simulations. The main goal is to reconstruct the energy scale within a 2% uncertainty.

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“…In this review we consider the LSND [1,2], Gallium [3][4][5][6][7] and reactor [8-10] short-baseline neutrino oscillation anomalies and we discuss their explanation in the framework of an effective 3+1 mixing scheme with one sterile neutrino at the eV scale (see Ref. [11]).…”

mentioning

confidence: 99%