Limits on neutrino oscillations in the appearance channels vμ → ve and vμ → ve

Armbruster, B.; Bodmann, B. E. J.; Blair, I.M.; Booth, N. E.; Dodd, A.C.; Drexlin, G.; Eberhard, V.; Edgington, J.A.; Eitel, K.; Ferstl, M.; Finckh, E.; Gemmeke, H.; Grandegger, W.; Höβ, J.; Jannakos, T.; Kleifges, M.; Kleinfeller, J.; Kretschmer, W.; Maschuw, R.; Rapp, J.; Plischke, P.; Schilling, F. P.; Seligmann, B.; Stumm, O.; Wolf, J.; Wölfle, S.; Zeitnitz, B.

doi:10.1016/0920-5632(94)00752-h

Cited by 19 publications

(19 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…LSND has attributed an excess of events above background toν µ →ν e , although these events have also been interpreted as an upper limit [12]. The KARMEN [15] experiment, which is similar to LSND in its sensitivity to δm 2 and mixing angle, has not yet accumulated enough data to convincingly confirm or rule out the LSND result. But perhaps the strongest indication of oscillations comes from the deficit of muons in the interactions of upward going atmospheric neutrinos, as recently reported by the SuperKamiokande collaboration [16].…”

Section: Introductionmentioning

confidence: 99%

Prospects for detecting supernova neutrino flavor oscillations

1999

View full text Add to dashboard Cite

The neutrinos from a Type II supernova provide perhaps our best opportunity to probe cosmologically interesting muon and/or tauon neutrino masses. This is because matter enhanced neutrino oscillations can lead to an anomalously hot ν e spectrum, and thus to enhanced charged current cross sections in terrestrial detectors. Two recently proposed supernova neutrino observatories, OMNIS and LAND, will detect neutrons spalled from target nuclei by neutral and charged current neutrino interactions. As this signal is not flavor specific, it is not immediately clear whether a convincing neutrino oscillation signal can be extracted from such experiments. To address this issue we examine the responses of a series of possible light and heavy mass targets, 9 Be, 23 Na, 35 Cl, and 208 Pb. We find that strategies for detecting oscillations which use only neutron count rates are problematic at best, even if cross sections are determined by ancillary experiments. Plausible uncertainties in supernova neutrino spectra tend to obscure rate enhancements due to oscillations. However, in the case of 208 Pb, a signal emerges that is largely flavor specific and extraordinarily sensitive to the ν e temperature, the emission of two neutrons. This signal and its flavor specificity are associated with the strength and location of the first-forbidden responses for neutral and charge current reactions, aspects of the 208 Pb neutrino cross section that have not been discussed previously. Hadronic spin transfer experiments might be helpful in confirming some of the nuclear structure physics underlying our conclusions. 14.60.Pq, 26.50.+x, 25.30.Pt

show abstract

Section: Introductionmentioning

confidence: 99%

Prospects for detecting supernova neutrino flavor oscillations

1999

View full text Add to dashboard Cite

show abstract

“…For the experiments searching for ν µ → ν e andν µ →ν e oscillations, we used the experiments E776 [7], KARMEN [8] and LSND [9] accelerator experiments;…”

Section: B Terrestrial Neutrinosmentioning

confidence: 99%

“…In the terrestrial neutrino experiments, many experimental groups have tried to observe the neutrino oscillations. The E531 [5], CHORUS and NOMAD [6] experiments using the beam from accelerators search for ν τ appearance in ν µ , and E776 [7], KARMEN [8] and LSND [9] experiments using the accelerator beams are searching for ν µ → ν e andν µ →ν e oscillations. The experiments using nuclear power reactor [10,11] search for the disappearance ofν e , in whichν e →ν X (X = µ, τ ) transitions are expected.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric Neutrino Oscillations in Three-Flavor Neutrinos

Sakai¹,

Teshima²

1999

Progress of Theoretical Physics

View full text Add to dashboard Cite

We analyze the atmospheric neutrino experiments of SuperKamiokande including zenith angle dependences using the three-flavor neutrino framework with the hierarchy m 2 1 ≈ m 2 2 m 2 3 . Taking into account the terrestrial, solar neutrino experimental data and the atmospheric neutrino experiments, including the sub-GeV and multi-GeV data in Su-perKamiokande, a large angle solution in the solar neutrino experiments is favored and the range of the mass parameter ∆m 2 23 is restricted in the range 0.08 eV 2 -2 eV 2 . Allowed regions of mixing parameters are θ 13 < 4 • , 27 • < θ 23 < 32 • for ∆m 2 23 = 1 eV 2 and θ 13 < 3 • , 28 • < θ 23 < 33 • for ∆m 2 23 = 0.1 eV 2Downloaded from 148 T. Teshima and T. Sakai m 3 partially including the zenith angle dependences. In this work, we perform the full analysis of zenith angle dependences in a SuperKamiokande atmospheric neutrino experiment 2) and analysis of Chooz data 11) in terrestrial experiment.In the three-flavor neutrino framework with the hierarchy m 1 ≈ m 2 m 3 , there are 5 parameters, sin 2 2θ 12 , θ 13 , θ 23 , ∆m 2 12 = m 2 2 − m 2 1 and ∆m 2 23 = m 2 3 − m 2 2 , concerned with neutrino oscillation. For solar neutrino deficit, the MSW solution 13), 14), 12) taking into account the matter effects predicts the large angle solution sin 2 2θ 12 = 0.6-0.9, ∆m 2 12 = 4 × 10 −6 -7 × 10 −5 eV 2 and small angle solution sin 2 2θ 12 = 0.003-0.01, ∆m 2 12 = 3 × 10 −6 -1.2 × 10 −5 eV 2 for θ 13 = 0 • -20 • . These large angle and small angle solutions are merged for θ 13 = 25 • -50 • . The vacuum solution for solar neutrinos is obtained as ∆m 2 12 ∼ 10 −10 eV 2 . 15) In terrestrial neutrino experiments, Fogli et al. 16) have thoroughly analyzed these experimental data and obtained the allowed regions in the tan θ 2 13 -tan 2 θ 23 plane for various values of the mass parameter ∆m 2 23 . We also analyzed the terrestrial neutrino experiments, 12) in which we have not included the Chooz experiment, and obtained results similar to those of Fogli et al. The allowed region in the tan 2 θ 13 -tan 2 θ 23 plane so obtained, for example for ∆m 2 23 = 0.02 eV 2 , is tan 2 θ 13 > 25, tan 2 θ 13 < 0.04 for all values of tan 2 θ 23 . For higher values of ∆m 2 23 , the allowed region in the tan 2 θ 13 -tan 2 θ 23 plane is more restricted, and for lower values, the allowed region spreads out, and for ∆m 2 23 < 0.001 eV 2 there is no restriction in the tan 2 θ 13 -tan 2 θ 23 plane. Atmospheric neutrino experiments have been analyzed in the three-flavor neutrino framework with the neutrino mass hierarchy m 1 ≈ m 2 m 3 by many authors. 17), 18), 12) The atmospheric neutrino anomaly of Kamiokande experiments 19) has been explained by ν µ ↔ ν τ oscillation with ∆m 2 23 ∼ 10 −2 -10 −1 eV 2 . These discussions contain the zenith angle dependences of sub-GeV and/or multi-GeV Kamiokande data. The zenith angle dependences in recent SuperKamiokande atmospheric experiments 1), 2) have decreasing character not only for the multi-GeV experiment but also for sub-GeV experiment. We have analyzed these depe...

show abstract

“…The LSND [33] collaboration claim a positive signal forν µ →ν e in an appearance experiment (L/E ≃ 0.98 m/MeV), with an appearance probability P (μ →ē) ≃ (0.31 ± 0.10 ± 0.05)%. The LSND result is plotted in Figure 5, together with the upper limits given by KARMEN [35] (L/E ≃ 0.44 m/MeV) and BNL-776 [36] (L/E ≃ 0.71 km/GeV). The curve shows the predicted appearance probability in threefold maximal mixing, plotted as a function of L/E, assuming ∆m 2 ≃ 0.72 × 10 −2 eV 2 [3].…”

Section: Accelerator and Reactor Experimentsmentioning

confidence: 99%

“…The LSND result [33] is indicated together with the upper limit obtained by Hill [34] from a subset of the LSND data. Upper limits from KARMEN [35] and BNL-776 [36] are shown, together with the projected sensitivities (90% upper limits, assuming no signal) of the CHORUS [38] and NOMAD [39] experiments. Figure 6.…”

Section: Aknowledgementmentioning

confidence: 99%

Further evidence for threefold maximal lepton mixing and a hierarchical spectrum of neutrino mass-squared differences

1997

View full text Add to dashboard Cite

The phenomenological case for threefold maximal lepton mixing is strengthened by more detailed comparison with existing data. The atmospheric neutrino data are self-consistent and in good agreement with the threefold maximal mixing prediction R = 2/3 (χ 2 /DOF = 4.3/5, CL = 51%). Including partiallycontained event data, the zenith angle dependence also points to threefold maximal mixing, ruling out a range of mixing schemes, including that of Fritzsch and Xing. Accounting for de facto uncertainties in solar neutrino fluxes, the solar neutrino data (including HOMESTAKE) are shown to be consistent with threefold maximal mixing (χ 2 /DOF = 5.1/3, CL = 16%), as is the upper limit from the LSND appearance experiment. Detailed predictions for forthcoming long-base-line reactor and accelerator experiments are presented.

show abstract

Limits on neutrino oscillations in the appearance channels vμ → ve and vμ → ve

Cited by 19 publications

References 4 publications

Prospects for detecting supernova neutrino flavor oscillations

Prospects for detecting supernova neutrino flavor oscillations

Atmospheric Neutrino Oscillations in Three-Flavor Neutrinos

Further evidence for threefold maximal lepton mixing and a hierarchical spectrum of neutrino mass-squared differences

Contact Info

Product

Resources

About