High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

Sinegovskaya, T. S.; Morozova, A.; Sinegovsky, S. I.

doi:10.1103/physrevd.91.063011

Cited by 40 publications

(27 citation statements)

References 60 publications

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“…In addition, we compare to other 1D muon [66] and neutrino flux [86] calculations that rely on numerical methods [73,74]. There, hadronic interactions are parameterized inclusively using tabulated secondary spectra.…”

Section: Impact Of the Improved Sibyll-23c On Inclusive Flux Calmentioning

confidence: 99%

Hadronic interaction model sibyll2.3cand inclusive lepton fluxes

et al. 2019

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Muons and neutrinos from cosmic ray interactions in the atmosphere originate from decays of mesons in air-showers. Sibyll-2.3c aims to give a precise description of hadronic interactions in the relevant phase space for conventional and prompt leptons in light of new accelerator data, including that from the LHC. Sibyll is designed primarily as an event generator for use in simulation of extensive air showers. Because it has been tuned for forward physics as well as the central region, it can also be used to calculate inclusive fluxes. The purpose of this paper is to describe the use of Sibyll-2.3c for calculation of fluxes of atmospheric leptons.

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Section: Impact Of the Improved Sibyll-23c On Inclusive Flux Calmentioning

confidence: 99%

Hadronic interaction model sibyll2.3cand inclusive lepton fluxes

et al. 2019

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“…[7], we consider the calculation of the conventional (mainly from π and K decays) and prompt (from charmed meson decays) atmospheric neutrino fluxes of Refs. [179][180][181][182] based on the Hillas and Gaisser (HGm) cosmicray approximation [183,184] and the hadronic model of Kimel and Mokhov (KM) [185], with updated parameters [186][187][188] for the conventional flux. We use the Zatsepin and Sokolskaya cosmic-ray model (ZS) [189] and the quark-gluon string model (QGSM) [190][191][192][193] for the prompt flux.…”

Section: B Improvements On the Calculation Of The Backgroundsmentioning

confidence: 99%

Analysis of the 4-year IceCube high-energy starting events

2016

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After four years of data taking, the IceCube neutrino telescope has detected 54 high-energy starting events (HESE, or contained-vertex events) with deposited energies above 20 TeV. They represent the first ever detection of high-energy extraterrestrial neutrinos and therefore, the first step in neutrino astronomy. In order to study the energy, flavor and isotropy of the astrophysical neutrino flux arriving at Earth, we perform different analyses of two different deposited energy intervals, [10 TeV − 10 PeV] and [60 TeV − 10 PeV]. We first consider an isotropic unbroken power-law spectrum and constrain its shape, normalization and flavor composition. Our results are in agreement with the preliminary IceCube results, although we obtain a slightly softer spectrum. We also find that current data are not sensitive to a possible neutrino-antineutrino asymmetry in the astrophysical flux. Then, we show that although a two-component power-law model leads to a slightly better fit, it does not represent a significant improvement with respect to a single powerlaw flux. Finally, we analyze the possible existence of a North-South asymmetry, hinted at by the combination of the HESE sample with the through-going muon data. If only using HESE data, the scarce statistics from the northern hemisphere does not allow us to reach any conclusive answer, which indicates that the HESE sample alone is not driving the potential North-South asymmetry.

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“…For Φ conventional ν l +ν l and Φ prompt ν l +ν l , when l = e, µ, we adopt the corresponding parametrizations from [44] and set Φ conventional give tracks. It is apparent that the probability that a resonance event will manifest itself as a shower highly boosted along the incident neutrino path is given by Γ(W → hadrons) + Γ(W → ν e e) + Γ(W → ν τ τ ) Γ(W → all) ≃ 0.9 (7) and the probability for observing a track is…”

Section: Experimental Observabilitymentioning

confidence: 99%

Hidden Glashow resonance in neutrino–nucleus collisions

Alikhanov

2016

Physics Letters B

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Today it is widely believed that s-channel excitation of an on-shell W boson, commonly known as the Glashow resonance, can be initiated in matter only by the electron antineutrino in the processν e e − → W − at the laboratory energy around 6.3 PeV. In this Letter we argue that the Glashow resonance within the Standard Model also occurs in neutrino-nucleus collisions. The main conclusions are as follows. 1) The Glashow resonance can be excited by both neutrinos and antineutrinos of all the three flavors scattering in the Coulomb field of a nucleus. 2) The Glashow resonance in a neutrino-nucleus reaction does not manifest itself as a Breit-Wigner-like peak in the cross section but the latter exhibits instead a slow logarithmic-law growth with the neutrino energy. The resonance turns thus out to be hidden. 3) More than 98% of W bosons produced in the sub-PeV region in neutrino-initiated reactions in water/ice will be from the Glashow resonance. 4) The vast majority of the Glashow resonance events in a neutrino detector is expected at energies from a few TeV to a few tens of TeV, being mostly initiated *

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High-energy neutrino fluxes and flavor ratio in the Earth’s atmosphere

Cited by 40 publications

References 60 publications

Hadronic interaction model sibyll2.3cand inclusive lepton fluxes

Hadronic interaction model sibyll2.3cand inclusive lepton fluxes

Analysis of the 4-year IceCube high-energy starting events

Hidden Glashow resonance in neutrino–nucleus collisions

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