Publisher’s Note: Precision Measurement of Neutrino Oscillation Parameters with KamLAND [Phys. Rev. Lett.<b>100</b>, 221803 (2008)]

Abe, S.; Ebihara, T.; Enomoto, S.; Furuno, K.; Gando, Y.; Ichimura, Kunihiro; Ikeda, H.; Inoue, K.; Kibe, Y.; Kishimoto, Y.; Koga, M.; Shimizu, Yusuke; Kozlov, A.; Minekawa, Y.; Mitsui, Tadao; Nakajima, K.; Nakamura, K.; Nakamura, Makoto; Owada, K.; Shimizu, I.; Shirai, J.; Suekane, F.; Suzuki, A.; Takemoto, Y.; Tamae, K.; Terashima, A.; Watanabe, Hiroko; Yonezawa, E.; Yoshida, Shigeru; Busenitz, J.; Classen, T.; Grant, C.; Keefer, G.; Leonard, D. S.; McKee, D.; Piepke, A.; Decowski, M. P.; Detwiler, J. A.; Freedman, S. J.; Fujikawa, B. K.; Gray, F.; Guardincerri, E.; Hsu, L.; Kadel, R.W.; Lendvai, C.; Luk, K. B.; Murayama, Hitoshi; O’Donnell, T.; Steiner, H. M.; Winslow, L. A.; Dwyer, D. A.; Jillings, C.; Mauger, C.; McKeown, R. D.; Vogel, P.; Zhang, C.; Berger, B. E.; Lane, C. E.; Maricic, J.; Miletic, T.; Batygov, M.; Learned, J. G.; Matsuno, S.; Pakvasa, Sandip; Foster, J. M.; Horton-Smith, G. A.; Tang, Alfred; Dazeley, S.; Downum, K. E.; Gratta, G.; Tolich, K.; Bugg, W.; Efremenko, Y. V.; Kamyshkov, Y.; Perevozchikov, O.; Karwowski, H. J.; Markoff, D. M.; Tornow, W.; Heeger, K. M.; Piquemal, F.; Ricol, J. S.

doi:10.1103/physrevlett.101.259901

Cited by 142 publications

(266 citation statements)

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“…The minimal Standard Model (SM) features massless neutrinos. However, the experimental observation of neutrino oscillations has established that at least two of the three known neutrinos are massive [1][2][3][4][5][6][7][8][9][10][11][12]. These experiments have measured the squared-mass differences ∆m 2 21 ≡ m 2 2 − m 2 1 and |∆m 2 32 | ≡ |m 2 3 − m 2 2 |, but are unable to probe the absolute neutrino mass scale.…”

mentioning

confidence: 99%

Radiative neutrino mass model from a mass dimension-11 ∆L = 2 effective operator

Gargalionis

Popa-Mateiu

Volkas

2020

J. High Energ. Phys.

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We present the first detailed phenomenological analysis of a radiative Majorana neutrino mass model constructed from opening up a ∆L = 2 mass-dimension-11 effective operator constructed out of standard model fields. While three such operators are generated, only one dominates neutrino mass generation, namely O 47 = L C LQ C QQQ C HH, where L denotes lepton doublet, Q quark doublet and H Higgs doublet. The underlying renormalisable theory contains the scalars S 1 ∼ (3, 1, 1/3) coupling as a diquark, S 3 ∼ (3, 3, 1/3) coupling as a leptoquark, and Φ 3 ∼ (3, 3, 2/3), which has no Yukawa couplings but does couple to S 1 and S 3 in addition to the gauge fields. Neutrino masses and mixings are generated at two-loop order. A feature of this model that is different from many other radiative models is the lack of proportionality to any quark and charged-lepton masses of the neutrino mass matrix. One consequence is that the scale of new physics can be as high as 10 7 TeV, despite the operator having a high mass dimension. This raises the prospect that ∆L = 2 effective operators at even higher mass dimensions may, when opened up, produce phenomenologically-viable radiative neutrino mass models. The parameter space of the model is explored through benchmark slices that are subject to experimental constraints from charged lepton flavour-violating decays, rare meson decays and neutral-meson mixing. The acceptable parameter space can accommodate the anomalies in R K ( * ) and the anomalous magnetic moment of the muon.

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mentioning

confidence: 99%

Radiative neutrino mass model from a mass dimension-11 ∆L = 2 effective operator

Gargalionis

Popa-Mateiu

Volkas

2020

J. High Energ. Phys.

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“…For the solar neutrino data, we perform a statistical analysis with the full spectral data from Super-Kamiokande phases I, III and IV [23][24][25], the combined analysis of all three SNO phases [26], Borexino [27], combined Gallex+GNO [41], SAGE [42] and Homestake [43]. For KamLAND data we used their 2008 spectral data [44].…”

Section: Complete Statistical Analysismentioning

confidence: 99%

Solar neutrino limits on decoherence

Holanda¹

2020

J. Cosmol. Astropart. Phys.

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The solar neutrino flux arrives at Earth as an incoherent admixture of mass eigenstates, and then solar neutrino detection constitute a blind probe to the oscillation pattern of the neutrino flavour conversion. Consequently, it is also impossible to probe, in a model independent approach, any new physics that leads to an enhancement of decoherence during the neutrino evolution, an effect that is present for instance in Open Quantum System formalism. However, such mechanism can also induce changes between mass eigenstates if an energy interchange between the neutrino subsystem and the reservoir is not explicitly forbiden. In this work the conversion probabilities between mass eigenstates in an Open Quantum System are calculated, and limits are stablished for these kind of transitions. We present our results in a pedagogical way, pointing out how far the analysis can go without any assumption on the neutrino conversion physics inside the Sun, before performing the full calculations. We obtain as limits for the decoherence parameters the values of Γ 3 < 6.5 × 10 −19 eV and Γ 8 < 7.1 × 10 −19 eV at 3σ.

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“…The position resolution for the 2.506 MeV γ from the 60 Co source is 19 cm, scaled as 30/ (E[MeV]) cm with energy [163]. More detail can be found in [136,166].…”

Section: Kamland Experimentsmentioning

confidence: 99%

“…KamLAND presented its first results on reactor antineutrino oscillations with the 162 t·yr exposure in 2003 [167]. The next analyses used exposure of 766 t·yr [168] and 2.881 kt·yr [166] respectively. In the latter analysis the statistical significance of spectral distortions exceeded the 5σ level, and the analysis of the reactor spectra was performed from the IBD threshold including among others the geoneutrino contribution.…”

Section: Kamland Experimentsmentioning

confidence: 99%

Experimental aspects of geoneutrino detection: Status and perspectives

Smirnov

2019

Progress in Particle and Nuclear Physics

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Neutrino geophysics, the study of the Earth's interior by measuring the fluxes of geologically produced neutrino at its surface, is a new interdisciplinary field of science, rapidly developing as a synergy between geology, geophysics and particle physics. Geoneutrinos, antineutrinos from longlived natural isotopes responsible for the radiogenic heat flux, provide valuable information for the chemical composition models of the Earth. The calculations of the expected geoneutrino signal are discussed, together with experimental aspects of geoneutrino detection, including the description of possible backgrounds and methods for their suppression. At present, only two detectors, Borexino and KamLAND, have reached sensitivity to the geoneutrino. The experiments accumulated a set of ∼190 geoneutrino events and continue the data acquisition. The detailed description of the experiments, their results on geoneutrino detection, and impact on geophysics are presented. The start of operation of other detectors sensitive to geoneutrinos is planned for the near future: the SNO+ detector is being filled with liquid scintillator, and the biggest ever 20 kt JUNO detector is under construction. A review of the physics potential of these experiments with respect to the geoneutrino studies, along with other proposals, is presented. New ideas and methods for geoneutrino detection are reviewed.

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Publisher’s Note: Precision Measurement of Neutrino Oscillation Parameters with KamLAND [Phys. Rev. Lett.100, 221803 (2008)]

Cited by 142 publications

References 0 publications

Radiative neutrino mass model from a mass dimension-11 ∆L = 2 effective operator

Radiative neutrino mass model from a mass dimension-11 ∆L = 2 effective operator

Solar neutrino limits on decoherence

Experimental aspects of geoneutrino detection: Status and perspectives

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