Search for neutrino oscillations on a long base-line at the CHOOZ nuclear power station

Apollonio, M.; Baldini, A.; Bemporad, C.; Caffau, E.; Cei, F.; Déclais, Y.; Kerret, H. de; Dieterle, B.; Etenko, A.; Foresti, L.; George, Jimin; Giannini, G.; Grassi, M.; Kozlov, Yu. V.; Kropp, W. R.; Kryn, D.; Laiman, M.; Lane, C.; Lefièvre, B.; Machulin, I.; Martemyanov, A.; Martemyanov, V. P.; Mikaelyan, L.A.; Nicoló, D.; Obolensky, M.; Pazzi, R.; Pieri, G.; Price, L. R.; Riley, S.; Reeder, R. A.; Sabelnikov, A.; Santin, G.; Skorokhvatov, M.; Sobel, H. W.; Steele, J.; Steinberg, R.; Sukhotin, S.; Tomshaw, S.; Véron, D.; Vyrodov, V.

doi:10.1140/epjc/s2002-01127-9

Cited by 929 publications

(651 citation statements)

References 27 publications

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“…When needed, we fix ∆m 2 ≃ 2.4 × 10 −3 eV 2 from atmospheric and accelerator data [37], sin 2 θ 12 ≃ 0.3 from reactor and solar data [35], and take representative value of sin 2 θ 13 below current upper bounds [38]. Matter effects are potentially relevant when the potential equals the neutrino wavenumber…”

Section: Overview Of Calculationsmentioning

confidence: 99%

Probing supernova shock waves and neutrino flavour transitions in next-generation water Cherenkov detectors

Fogli

Lisi

Mirizzi

et al. 2005

J. Cosmol. Astropart. Phys.

109

131

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Several current projects aim at building a large water-Cherenkov detector, with a fiducial volume about 20 times larger than in the current Super-Kamiokande experiment. These projects include the Underground nucleon decay and Neutrino Observatory (UNO) in the Henderson Mine (Colorado), the Hyper-Kamiokande (HK) detector in the Tochibora Mine (Japan), and the MEgaton class PHYSics (MEMPHYS) detector in the Fréjus site (Europe). We study the physics potential of a reference next-generation detector (0.4 Mton of fiducial mass) in providing information on supernova neutrino flavor transitions with unprecedented statistics. After discussing the ingredients of our calculations, we compute neutrino event rates from inverse beta decay (ν e p → e + n), elastic scattering on electrons, and scattering on oxygen, with emphasis on their time spectra, which may encode combined information on neutrino oscillation parameters and on supernova forward (and possibly reverse) shock waves. In particular, we show that an appropriate ratio of low-to-high energy events can faithfully monitor the time evolution of the neutrino crossing probability along the shock-wave profile. We also discuss some background issues related to the detection of supernova relic neutrinos, with and without the addition of gadolinium.

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Section: Overview Of Calculationsmentioning

confidence: 99%

Probing supernova shock waves and neutrino flavour transitions in next-generation water Cherenkov detectors

Fogli

Lisi

Mirizzi

et al. 2005

J. Cosmol. Astropart. Phys.

109

131

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“…Atmospheric neutrino studies [13], K2K [14] 3). The CHOOZ experiment [15] gives a bound θ 13 as a function of ∆m 2 31 . The physical effects involved in the interpretation are -vacuum oscillations [9,10,16] (atmospheric neutrinos -main mode, K2K, MINOS and CHOOZ); -the Mikheyev-Smirnov-Wolfenstein (MSW) effect -the adiabatic conversion [17,18] (conversion of solar neutrinos in the matter of the Sun; at low energies solar neutrinos undergo the averaged vacuum oscillation with small matter effect); and -oscillations in matter [17,18] (oscillations of solar and atmospheric neutrinos in the matter of Earth).…”

Section: Experimental Results and Global Fitsmentioning

confidence: 99%

“…In a certain basis, one of these two sets of Yukawa coupling matrices is diagonal, and the Yukawa sector has only nine parameters. Noting that the (2,2,15) submultiplet of 126 H as well as the (2,2,1) submultiplet of 10 H each have a pair of standard model doublets that contribute to charged-fermion masses, one can write the quark and lepton mass matrices as follows [137]: To generate the light neutrino masses, we use the seesaw formula in eq. (80), where f is the same 126 H Yukawa coupling as above.…”

Section: Neutrino Mass and New Physics: "Top-down"mentioning

confidence: 99%

Neutrino mass and New physics

Smirnov

2006

J. Phys.: Conf. Ser.

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We review the present state and future outlook of our understanding of neutrino masses and mixings. We discuss what we think are the most important perspectives on the plausible and natural scenarios for neutrinos and attempt to throw light onto the flavor problem of quarks and leptons. This review focuses on the seesaw mechanism, which fits into a big picture of particle physics such as supersymmetry and grand unification providing a unified approach to the flavor problem of quarks and leptons. We argue that in combination with family symmetries, this may be at the heart of a unified understanding of the flavor puzzle. We also discuss other new physics ideas such as neutrinos in models with extra dimensions and possible theoretical implications of sterile neutrinos. We outline some tests for the various schemes.

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“…Figure 3 summarises the information on θ 13 from present data, which emerges from an interplay of different data sets. An important contribution to the bound comes from the CHOOZ reactor experiment [57] combined with the determination of |∆m 2 31 | from atmospheric and long-baseline experiments. Using this set of data, a possible hint for a non-zero θ 13 from atmospheric data has been found in references [55,58].…”

Section: Neutrino Oscillation Updatementioning

confidence: 99%