Neutrino measurements with the IMB director

Becker‐Szendy, R.; Bratton, C. B.; Casper, D.; Dye, S. T.; Gajewski, W.; Ganezer, K. S.; Goldhaber, M.; Haines, T. J.; Halverson, P. G.; Kiełczewska, D.; Kropp, W. R.; Learned, J. G.; LoSecco, J. M.; McGrath, G.; McGrew, C.; Masuzawa, M.; Matsuno, S.; Miller, R. S.; Price, L. R.; Reines, F.; Schultz, J.; Sobel, H. W.; Stone, J. L.; Sulak, L.; Svoboda, R.

doi:10.1016/0920-5632(94)00765-n

Cited by 144 publications

(109 citation statements)

References 9 publications

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“…The first factor in the calculation is well-understood, and different calculations give similar results [11,12]. The uncertainty in the cross section is discussed in recent papers [13,14,15]. In this paper we discuss the calculation of the neutrino flux in the energy range relevant for neutrino-induced muons; that is, from one GeV up to 10 4 GeV of neutrino energy.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric neutrino flux above 1 GeV

et al. 1996

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In this paper we extend an earlier calculation of the flux of atmospheric neutrinos to higher energy. The earlier calculation of the neutrino flux below 3 GeV has been used for calculation of the rate of contained neutrino interactions in deep underground detectors. The fluxes are needed up to neutrino energies of 10 TeV to calculate the expected rate of neutrino-induced muons passing into and through large, deep detectors. We compare our results with several other calculations, and we evaluate the uncertainty in the rate of neutrino-induced muons due to uncertainties in the neutrino flux.

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Section: Introductionmentioning

confidence: 99%

Atmospheric neutrino flux above 1 GeV

et al. 1996

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“…On the other hand, the explanation of the atmospheric neutrino data with ν µ → ν τ oscillations [9][10][11][12][13], that is favored by the latest Super-Kamiokande data [65], requires a large mixing in the ν µ , ν τ -ν 3 , ν 4 sector which could be related to the fact that |U µ3 | 2 + |U µ4 | 2 and |U τ 3 | 2 + |U τ 4 | 2 are large (close to one) and m 3 ≃ m 4 . Therefore, in the following we will assume that |U e3 | 2 and |U e4 | 2 have different orders of magnitude.…”

Section: B Scheme Bmentioning

confidence: 99%

“…At present there are three experimental indications in favor of neutrino oscillations that have been obtained in solar neutrino experiments (Homestake [4], Kamiokande [5], GALLEX [6], SAGE [7] and Super-Kamiokande [8]), in atmospheric neutrino experiments (Kamiokande [9], IMB [10], Super-Kamiokande [11], Soudan-2 [12] and MACRO [13])) and in the accelerator LSND experiment [14,15]. On the other hand, neutrinoless double-β decay (ββ 0ν ) experiments [16][17][18][19] and the experiments on the direct measurement of neutrino masses [20] did not obtain any positive result so far (see [21]).…”

Section: Introductionmentioning

confidence: 99%

Neutrinoless double-β decay with three or four neutrino mixing

Giunti¹

2000

Phys. Rev. D

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Considering the scheme with mixing of three neutrinos and a mass hierarchy that can accommodate the results of solar and atmospheric neutrino experiments, it is shown that the results of solar neutrino experiments imply a lower bound for the effective Majorana mass in neutrinoless double-β decay, under the natural assumptions that massive neutrinos are Majorana particles and there are no unlikely fine-tuned cancellations among the contributions of the different neutrino masses. Considering the four-neutrino schemes that can accommodate also the results of the LSND experiment, it is shown that only one of them is compatible with the results of neutrinoless double-β decay experiments and with the measurement of the abundances of primordial elements produced in Big-Bang Nucleosynthesis. It is shown that in this scheme, under the assumptions that massive neutrinos are Majorana particles and there are no cancellations among the contributions of the different neutrino masses, the results of the LSND experiment imply a lower bound for the effective Majorana mass in neutrinoless double-β decay.

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“…Many experiments searching for neutrino oscillations and neutrinoless double-beta decay and investigating the high-energy part of the tritium beta-spectrum are going on or are under preparation. At present, indications that neutrinos are massive and mixed have been found in solar neutrino experiments (Homestake [5], Kamiokande [6], GALLEX [7], SAGE [8] and Super-Kamiokande [9,10]), in atmospheric neutrino experiments (Kamiokande [11], IMB [12], Soudan [13] and Super-Kamiokande [14,10]) and in the LSND experiment [15]. From the analyses of the data of these experiments in terms of neutrino oscillations it follows that there are three different scales of neutrino mass-squared differences: ∆m 2 sun ∼ 10 −5 eV 2 (MSW) or ∆m 2 sun ∼ 10 −10 eV 2 (vac.…”

Section: Introductionmentioning

confidence: 99%

Four-neutrino mixing and Big-Bang Nucleosynthesis

Bilenky¹,

Giunti²,

Grimus³

et al. 1999

Astroparticle Physics

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We investigate the Big-Bang Nucleosynthesis constraints on neutrino mixing in the framework of the two four-neutrino schemes that are favored by the results of neutrino oscillation experiments. We discuss the implications of these constraints for terrestrial short and long-baseline neutrino oscillation experiments and we present some possibilities of testing them in these experiments. In particular, we show that from the Big-Bang Nucleosynthesis constraints it follows that the (−) ν µ → (−) ν τ transition is severely suppressed in short-baseline experiments, whereas its oscillation amplitude in long-baseline experiments is of order 1. We also propose a new parameterization of the four-neutrino mixing matrix U which is appropriate for the schemes under consideration.

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Neutrino measurements with the IMB director

Cited by 144 publications

References 9 publications

Atmospheric neutrino flux above 1 GeV

Atmospheric neutrino flux above 1 GeV

Neutrinoless double-β decay with three or four neutrino mixing

Four-neutrino mixing and Big-Bang Nucleosynthesis

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