Atmospheric neutrino fluxes

Gaisser, T. K.

doi:10.1063/1.1361736

Cited by 2 publications

(2 citation statements)

References 13 publications

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“…Other important sources of uncertainties [20,21] in the determination of the allowed region for the oscillation parameters are the input primary spectra, where very valuable new data became recently available [22,23,24], and the modeling of hadronic interactions. New data on this problem would also be of great value [25].…”

Section: Discussionmentioning

confidence: 99%

The east–west effect for atmospheric neutrinos

Lipari¹

2000

Astroparticle Physics

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The atmospheric neutrino fluxes observed by underground detectors are not symmetric for rotations around the vertical axis. The flux is largest (smallest) for the ν's traveling toward east (west). This asymmetry is the result of the effects of the geomagnetic field on the primary cosmic rays and on their showers. The size of the asymmetry is to a good approximation independent from the existence of neutrino oscillations, and can in principle be predicted without any ambiguity due to existence of unknown new physics. We show that there is an interesting hint of discrepancy between the experimental measurement of the east-west asymmetry by Super-Kamiokande and the existing theoretical predictions. We argue that the discrepancy is a real effect caused by the neglect, in the existing calculations, of the bending of the charged secondary particles (in particular of the muons) in the cosmic ray showers. The inclusion of this effect in the calculation gives results in quantitative agreeement with the data. We comment on the implications of this result for the study of neutrino oscillations.

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Section: Discussionmentioning

confidence: 99%

The east–west effect for atmospheric neutrinos

Lipari¹

2000

Astroparticle Physics

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“…spheric muons and atmospheric neutrinos, although the systematic uncertainties in flux are rather large at the energies of interest. T. Gaisser 119 has estimated the uncertainty in the absolute neutrino flux to be 30%, which is dominated by two components: the uncertainty in the flux of the primary cosmic rays and uncertainty in the kaon production cross section. AMANDA captures neutrino-induced muons with energies between 50 GeV and somewhat larger than 2 TeV (see fig.…”

Section: Number Of Channelsmentioning

confidence: 99%

The Proceedings of the 28th SLAC Summer Institute on Particle Physics: Neutrinos From The Lab, The Sun, And The Cosmos (SSI 2000)

Jaros¹

2004

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Interest in cosmic sources of high energy neutrinos dates back to the late 1950's. This paper outlines the interdisciplinary scientific agenda, which span the fields of astronomy, particle physics, and cosmic ray physics. While the general detection principles based on optical Cherenkov radiation have been understood for many years, the unusual geographic locations of suitable detector sites have challenged the ingenuity of experimentalists. Two high energy neutrino programs are now operating (NT200 in Lake Baikal and the AMANDA detector), with the expectation of ushering in the era of multi-messenger astronomy. Two Mediterranean-based programs have made impressive progress. These detectors are optimized to detect neutrinos with energies of the order of 1-10 TeV, although they are capable of detecting neutrinos over a much broader range of energies. For E > 10 15 eV, several new ideas are being exploited to expand the effective volume of the detector. These techniques are based on the detection of neutrino-initiated cascades. We describe the ongoing worldwide efforts to develop expandable techniques and offer an assessment of their relative capabilities.

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Atmospheric neutrino fluxes

Abstract: Starting with an historical review, I summarize the status of calculations of the flux of atmospheric neutrinos and how they compare to the measurements.

Cited by 2 publications

References 13 publications

The east–west effect for atmospheric neutrinos

The east–west effect for atmospheric neutrinos

The Proceedings of the 28th SLAC Summer Institute on Particle Physics: Neutrinos From The Lab, The Sun, And The Cosmos (SSI 2000)

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