Electroweak tests at beta-beams

Balantekin, A. B.; Jesus, J. H. de; Volpe, Cristina

doi:10.1016/j.physletb.2006.01.059

Cited by 39 publications

(64 citation statements)

References 26 publications

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“…Second, the depth of modulation in this model is too small. In the Super-Kamiokande energy region the predicted [12] modulation is ∼ 2-3%, but we find about 7%. Third, the depth of modulation is predicted [12] to increase with neutrino energy, being 0.77% at 2.50 MeV and 1.03% at 3.35 MeV, whereas we find large effects at low energy; see Fig.…”

Section: Significance For Neutrino Physicscontrasting

confidence: 67%

Evidence for solar neutrino flux variability and its implications

Caldwell

Sturrock

2005

Astroparticle Physics

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Although KamLAND apparently rules out Resonant-Spin-Flavor-Precession (RSFP) as an explanation of the solar neutrino deficit, the solar neutrino fluxes in the Cl and Ga experiments appear to vary with solar rotation. Added to this evidence, summarized here, a power spectrum analysis of the Super-Kamiokande data reveals significant variation in the flux matching a dominant rotation rate observed in the solar magnetic field in the same time period. Three frequency peaks, all related to this rotation rate, can be explained quantitatively. A Super-Kamiokande paper reported no time variation of the flux, but showed the same peaks, there interpreted as statistically insignificant, due to an inappropriate analysis. This modulation is small (7%) in the Super-Kamiokande energy region (and below the sensitivity of the Super-Kamiokande analysis) and is consistent with RSFP as a subdominant neutrino process in the convection zone. The data display effects that correspond to solar-cycle changes in the magnetic field, typical of the convection zone. This subdominant process requires new physics: a large neutrino transition magnetic moment and a light sterile neutrino, since an effect of this amplitude occurring in the convection zone cannot be achieved with the three known neutrinos. It does, however, resolve current problems in providing fits to all experimental estimates of the mean neutrino flux, and is compatible with the extensive evidence for solar neutrino flux variability.

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Section: Significance For Neutrino Physicscontrasting

confidence: 67%

Evidence for solar neutrino flux variability and its implications

Caldwell

Sturrock

2005

Astroparticle Physics

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“…Neutrino-electron elastic scattering offers an ideally clean setting for this measurement, which is competitive at a high energy neutrino factory [3], but (because the cross section grows linearly with the energy) at a low-energy facility very high intensities are required [6]. A measurement of the Weinberg angle can be obtained from the CC/NC deep-inelastic scattering ratio: this measurement at present is almost competitive, but marred by the uncertainty related to parton distributions [7].…”

Section: The Weinberg Angle From Neutrinonucleon Elastic Scatteringmentioning

confidence: 99%

Tests of the Standard Model with Low–Energy Neutrino Beams

Antonelli

Battistoni

Ferrario

et al. 2007

Nuclear Physics B - Proceedings Supplements

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“…The experiments with the NNS can be carried out using the intense, pulsed spallation sources, beta-beams facilities, superbeams and neutrino factories [10,11,12,13]. Various applications of the neutrino beams in area of the NNS and SM tests have been discussed in literature [14,15,16,17,18]. Although the SM agrees with the experimental data up to available energies, there are numerous theoretical reasons for which it can not be viewed as a ultimate theory.…”

Section: Introductionmentioning

confidence: 97%

T-odd correlation in muon neutrino elastic scattering on polarized proton target

Sobków

2013

Nuclear Physics B

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In this paper, we analyze the elastic scattering of the muon neutrino beam on the polarized proton target (PPT), and predict how the existence of CPviolating phase between the complex vector V and axial A couplings of the left-chirality neutrinos affects the azimuthal dependence of the differential cross section. The neutrinos are assumed to be Dirac fermions with non-zero mass. We show that the azimuthal asymmetry of recoil protons does not depend on the neutrino mass and does not vanish even if β V A = 0. The CPbreaking phase β V A could be detected by measuring the maximal asymmetry of the differential cross section. We also indicate the possibility of using the PPT to distinguish the detector background from the neutrino interactions. Our analysis is model-independent and the results are presented in a limit of infinitesimally small neutrino mass.

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Electroweak tests at beta-beams

Cited by 39 publications

References 26 publications

Evidence for solar neutrino flux variability and its implications

Evidence for solar neutrino flux variability and its implications

Tests of the Standard Model with Low–Energy Neutrino Beams

T-odd correlation in muon neutrino elastic scattering on polarized proton target

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