Masses and mixings from neutrino beams pointing to neutrino telescopes

Dick, K.; Freund, M.; Lindner, M.

doi:10.1016/s0550-3213(00)00512-5

Cited by 9 publications

(5 citation statements)

References 15 publications

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“…[4,6,43]). It requires sufficiently strong matter effects, which implies the need for a very long baseline (> 1 000 km) together with an energy close to the MSW-resonance energy of about 10 to 15 GeV [54]. Because the degenerate solution also implies a different value of δ CP , smaller CP-effects in the second oscillation maximum would eliminate the CP-phase as a parameter of the measurement and could help to measure the sign of ∆m 2 31 .…”

Section: The Sign Of ∆M 2 31 Sensitivitymentioning

confidence: 99%

Superbeams vs. neutrino factories

2002

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We compare the physics potential of planned superbeams with the one of neutrino factories. Therefore, the experimental setups as well as the most relevant uncertainties and errors are considered on the same footing as much as possible. We use an improved analysis including the full parameter correlations, as well as statistical, systematical, and degeneracy errors. Especially, degeneracies have so far not been taken into account in a numerical analysis. We furthermore include external input, such as improved knowledge of the solar oscillation parameters from the KamLAND experiment. This allows us to determine the limiting uncertainties in all cases. For a specific comparison, we choose two representatives of each class: For the superbeam, we take the first conceivable setup, namely the JHF to SuperKamiokande experiment, as well as, on a longer time scale, the JHF to Hyper-Kamiokande experiment. For the neutrino factory, we choose an initially conceivable setup and an advanced machine. We determine the potential to measure the small mixing angle sin 2 2θ 13 , the sign of ∆m 2 31 , and the leptonic CP phase δ CP , which also implies that we compare the limitations of the different setups. We find interesting results, such as the complete loss of the sensitivity to the sign of ∆m 2 31 due to degeneracies in many cases. * Work supported by "Sonderforschungsbereich 375 für Astro-Teilchenphysik" der Deutschen Forschungsgemeinschaft and the "Studienstiftung des deutschen Volkes" (German National Merit Foundation) [W.W.]. a

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Section: The Sign Of ∆M 2 31 Sensitivitymentioning

confidence: 99%

Superbeams vs. neutrino factories

2002

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“…With the medium energy beam and a baseline of 7300 km (Fermilab to Gran Sasso) only 17% of the pions decay within the channel. Hence, the channel length restrictions would exclude, or at least heavily penalize, the extremely-long-baseline ideas proposed by Dick et al [75]. Clearly, decay channel length restrictions must be taken into account when comparing choices of baseline and beam energy.…”

Section: Decay Channel Length Restrictionsmentioning

confidence: 99%

Exploring neutrino oscillations with superbeams

et al. 2001

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We consider the medium-and long-baseline oscillation physics capabilities of intense muon-neutrino and muon-antineutrino beams produced using future upgraded megawatt-scale high-energy proton beams. In particular we consider the potential of these conventional neutrino ''superbeams'' for observing → e oscillations, determining the hierarchy of neutrino mass eigenstates, and measuring CP violation in the lepton sector. The physics capabilities of superbeams are explored as a function of the beam energy, baseline, and the detector parameters ͑fiducial mass, background rates, and systematic uncertainties on the backgrounds͒. The trade-offs between very large detectors with poor background rejection and smaller detectors with excellent background rejection are illustrated. We find that, with an aggressive set of detector parameters, it may be possible to observe → e oscillations with a superbeam provided that the amplitude parameter sin 2 2 13 is larger than a few ϫ10 Ϫ3 . If sin 2 2 13 is of order 10 Ϫ2 or larger, then the neutrino mass hierarchy can be determined in long-baseline experiments, and if in addition the large mixing angle MSW solution describes the solar neutrino deficit, then there is a small region of parameter space within which maximal CP violation in the lepton sector would be observable ͑with a significance of a few standard deviations͒ in a low-energy mediumbaseline experiment. We illustrate our results by explicitly considering massive water Cherenkov and liquid argon detectors at superbeams with neutrino energies ranging from 1 GeV to 15 GeV, and baselines ranging from 295 km to 9300 km. Finally, we compare the oscillation physics prospects at superbeams with the corresponding prospects at neutrino factories. The sensitivity at a neutrino factory to CP violation and the neutrino mass hierarchy extends to values of the amplitude parameter sin 2 2 13 that are one to two orders of magnitude lower than at a superbeam.tions at a mass-squared-difference scale Ͼ10 Ϫ3 eV 2 with amplitude Ͼ0.1. Furthermore, large amplitude → s oscillations at the ␦m atm 2 scale are also excluded by SuperK. This is because → s oscillations are expected to be significantly affected by propagation through matter ͓7,8͔, causing a distortion in the zenith-angle distribution at large angles ͑corresponding to long path lengths͒ that is not present in the data ͓9͔. The zenith-angle distribution observed by SuperK excludes → s oscillations of maximal amplitude at 99% confidence level ͓9͔. We conclude that, if the oscillation interpretation of the atmospheric neutrino deficit is correct, the dominant mode must be → oscillation, with the possibility of some smaller amplitude muon-neutrino oscillations to sterile and/or electron-neutrinos ͓10͔.An exotic alternative interpretation ͓11͔ of the atmospheric neutrino disappearance results is that a neutrino mass eigenstate, which is a dominant component of the state, decays to a lighter mass-eigenstate and a Majoron ͓12͔. The first oscillation minimum in → must be observed or excluded t...

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“…have discussed electron neutrino appearance; however, the detection of a signal due to electrons is significantly more demanding than those due to muons. Ref [17]. discussed something closer to the present proposal; however, its authors have considered energy thresholds modeled on the existing neutrino telescopes, that are larger than our threshold: this has a significant impact on the ensuing conclusions.…”

mentioning

confidence: 79%

“…We have argued that the ideal conditions are obtained for muon neutrinos with average energies of 6 (8) GeV, that propagate for a distance of L = 6000 (8000) km. A previous similar proposal, [17], discussed larger detectors with higher energy thresholds modeled on neutrino telescopes; other apparently related proposals [15,16] considered electron neutrino detection instead, that is significantly more demanding than muon detection.…”

Section: Summary and Discussionmentioning

confidence: 99%

Counting muons to probe the neutrino mass spectrum

2013

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Abstract. The experimental evidence that θ13 is large opens new opportunities to identify the neutrino mass spectrum. We outline a possibility to investigate this issue by means of conventional technology. The ideal setup turns out to be long baseline experiment: the muon neutrino beam, with 10 20 protons on target, has an average energy of 6 (8) GeV; the neutrinos, after propagating 6000 (8000) km, are observed by a muon detector of 1 Mton and with a muon energy threshold of 2 GeV. The expected number of muon events is about 1000, and the difference between the two neutrino spectra is sizeable, about 30%. This allows the identification of the mass spectrum just counting muon tracks. The signal events are well characterized experimentally by their time and direction of arrival, and 2/3 of them are in a region with little atmospheric neutrino background, namely, between 4 GeV and 10 GeV. The distances from CERN to Baikal Lake and from Fermilab to KM3NET, or ANTARES, fit in the ideal range.

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Masses and mixings from neutrino beams pointing to neutrino telescopes

Cited by 9 publications

References 15 publications

Superbeams vs. neutrino factories

Superbeams vs. neutrino factories

Exploring neutrino oscillations with superbeams

Counting muons to probe the neutrino mass spectrum

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