Atmospheric neutrino flux above 1 GeV

Agrawal, Vivek; Gaisser, T. K.; Lipari, P.; Stanev, T.

doi:10.1103/physrevd.53.1314

Cited by 328 publications

(348 citation statements)

References 50 publications

(52 reference statements)

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“…Up-going atmospheric neutrinos from the decay of pions and kaons are simulated using the package GENHEN [28,29] assuming the model from the Bartol group [30,31] which does not include the decay of charmed particles. The analysis presented in this paper is based on a run-by-run Monte Carlo simulation [32], which takes into consideration the real data taking conditions of the detector (e.g.…”

Section: Background Simulationmentioning

confidence: 99%

Search for relativistic magnetic monopoles with five years of the ANTARES detector data

Albert

André

Anghinolfi

et al. 2017

J. High Energ. Phys.

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A search for magnetic monopoles using five years of data recorded with the ANTARES neutrino telescope from January 2008 to December 2012 with a total live time of 1121 days is presented. The analysis is carried out in the range β > 0.6 of magnetic monopole velocities using a strategy based on run-by-run Monte Carlo simulations. No signal above the background expectation from atmospheric muons and atmospheric neutrinos is observed, and upper limits are set on the magnetic monopole flux ranging from 5.7 × 10 −16 to 1.5 × 10 −18 cm −2 · s −1 · sr −1 .

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Section: Background Simulationmentioning

confidence: 99%

Search for relativistic magnetic monopoles with five years of the ANTARES detector data

Albert

André

Anghinolfi

et al. 2017

J. High Energ. Phys.

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“…At more modest energies, the angular and temporal resolution of a neutrino telescope will be needed to effectively remove backgrounds. The atmospheric neutrino flux at 1 TeV (dominated by ν µ +ν µ ) is ∼ 10 −8 GeV cm −2 s −1 [30] in a (1 deg) 2 bin, where the bin size was chosen to reflect the angular resolution for these events. Especially for the lower flux we consider below, identification of astrophysical sources may require temporal information as well.…”

Section: Basics First: Measuring the Neutrino Spectrum With Muonsmentioning

confidence: 99%

Erratum: Measuring flavor ratios of high-energy astrophysical neutrinos [Phys. Rev. D 68, 093005 (2003)]

Beacom¹,

Bell²,

Hooper³

et al. 2005

Phys. Rev. D

156

243

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We discuss the prospects for next generation neutrino telescopes, such as IceCube, to measure the flavor ratios of high-energy astrophysical neutrinos. The expected flavor ratios at the sources are φν e : φν µ : φν τ = 1 : 2 : 0, and neutrino oscillations quickly transform these to 1 : 1 : 1. The flavor ratios can be deduced from the relative rates of showers (νe charged-current, most ντ chargedcurrent, and all flavors neutral-current), muon tracks (νµ charged-current only), and tau lepton lollipops and double-bangs (ντ charged-current only). The peak sensitivities for these interactions are at different neutrino energies, but the flavor ratios can be reliably connected by a reasonable measurement of the spectrum shape. Measurement of the astrophysical neutrino flavor ratios tests the assumed production mechanism and also provides a very long baseline test of a number of exotic scenarios, including neutrino decay, CPT violation, and small-δm 2 oscillations to sterile neutrinos.PACS numbers: 95.85. Ry, 96.40.Tv, 13.35.Hb, 14.60.Pq

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“…The differential distribution of the atmospheric neutrino fluxes at Gran Sasso has been generated according to the predictions of the 1-D Bartol model [11]. Neutrino interactions have been calculated with GRV94 parton distributions [12] with explicit inclusion of the contribution of quasi-elastic scattering and of single pion production to the neutrino cross-sections [13].…”

Section: Experiments Simulationmentioning

confidence: 99%

Prospects of measuring $\sin^2 2\Theta_{13}$ and the sign of $\Delta m^2$ with a massive magnetized detector for atmospheric neutrinos

Fatis

Tabarelli²

2002

Eur. Phys. J. C

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Abstract. The pattern of oscillation parameters emerging from current experimental data can be further elucidated by the observation of matter effects. In contrast to planned experiments with conventional neutrino beams, atmospheric neutrinos offer the possibility to search for Earth-induced matter effects with very long baselines. Resonant matter effects are asymmetric on neutrinos and anti-neutrinos, depending on the sign of ∆m 2 . In a three-generation oscillation scenario, this gives access to the mass hierarchy of neutrinos, while the size of the asymmetry would measure the admixture of electron neutrinos to muon/tau neutrino oscillations (the mixing angle Θ13). The sensitivity to these effects is discussed after the detailed simulation of a realistic experiment based on a massive detector for atmospheric neutrinos with charge identification. We show how a detector, which measure and distinguish between νµ and νµ charged current events, might be sensitive to matter effects using atmospheric neutrinos, provided the mixing angle Θ13 is large enough.

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Atmospheric neutrino flux above 1 GeV

Cited by 328 publications

References 50 publications

Search for relativistic magnetic monopoles with five years of the ANTARES detector data

Search for relativistic magnetic monopoles with five years of the ANTARES detector data

Erratum: Measuring flavor ratios of high-energy astrophysical neutrinos [Phys. Rev. D 68, 093005 (2003)]

Prospects of measuring $\sin^2 2\Theta_{13}$ and the sign of $\Delta m^2$ with a massive magnetized detector for atmospheric neutrinos

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