Ultrahigh-energy neutrino interactions

Gandhi, Raj; Quigg, Chris; Reno, Mary Hall; Sarčević, Ina

doi:10.1016/0927-6505(96)00008-4

Cited by 582 publications

(687 citation statements)

References 106 publications

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“…We give the correspondence between integrated column depth of the Earth (see e.g. [33]) and zenith angle for several trajectories ending at the center of IceCube. We observe, for example, that whereas a muon of E = 10 7 GeV has a range of about 25 km water equivalent (w.e.)…”

Section: Background Of Muon Pairs and Signal At Icecubementioning

confidence: 99%

Long-lived staus from cosmic rays

Ahlers

Illana

Masip

et al. 2007

J. Cosmol. Astropart. Phys.

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The collision of a high energy cosmic ray with a nucleon in the upper atmosphere could produce long-lived heavy particles. Such particles would be very penetrating, since the energy loss in matter scales as the inverse mass, and could reach a neutrino telescope like IceCube from large zenith angles. Here we study this possibility and focus on the long-lived stau of SUSY models with a gravitino LSP. The signal would be a pair of muon-like parallel tracks separated by 50 meters along the detector. We evaluate the background of muon pairs and show that any events from zenith angles above 80 • could be explained by the production of these heavy particles by cosmic rays.

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Section: Background Of Muon Pairs and Signal At Icecubementioning

confidence: 99%

Long-lived staus from cosmic rays

Ahlers

Illana

Masip

et al. 2007

J. Cosmol. Astropart. Phys.

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“…where σ CC (νN/νN) is the neutrino-nucleon cross section which is ≈ 1.4 × 10 −33 cm 2 at E ν = 6.3 PeV [24]. For ν α N +ν α N (NC), the rate is calculated as…”

Section: Shower Signatures Of the Glashow Resonancementioning

confidence: 99%

“…Unlike the neutrino-nucleon charged current scattering ν µ N → µX (and its charge conjugated counterpart), the pure muon track is not accompanied by any shower activity at its starting point. We note that in ν µ N → µX processes with PeV neutrino energies, about 26% of the initial neutrino energy is transfered to the kicked quark, which turns into a hadronic cascade [24]. Thus, a muon track from ν µ N → µX is accompanied by a ∼ 200 m radius shower at the interaction vertex for PeV neutrino energies.…”

Section: Introductionmentioning

confidence: 99%

The Glashow resonance at IceCube: signatures, event rates andppvs.pγ interactions

Bhattacharya¹,

Gandhi²,

Rodejohann³

et al. 2011

J. Cosmol. Astropart. Phys.

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We revisit the signatures of the Glashow resonance processν e e → W in the highenergy astrophysical neutrino observatory IceCube. We note that in addition to the standard hadronic and electromagnetic showers produced by an incoming neutrino at the resonance energy of E ν ≈ 6.3 PeV, there are two clear signals of the process: the "pure muon" fromν e e →ν µ µ and the "contained lollipop" fromν e e →ν τ τ . The event rate and the signal-to-background ratio (the ratio of the resonant to concurrent non-resonant processes) are calculated for each type of interaction, based on current flux limits on the diffuse neutrino flux. Because of the low background in the neighborhood of the resonance, the observation of only one pure muon or contained lollipop event essentially signals discovery of the resonance, even if the expected event numbers are small. We also evaluate the total event rates of the Glashow resonance from the extra-galactic diffuse neutrino flux and emphasize its utility as a discovery tool to enable first observations of such a flux. We find that one can expect 3.6 (0.65) events per year for a pure pp (pγ) source, along with an added contribution of 0.51 (0.21) from non-resonant events. We also give results as a function of the ratio of pp vs pγ sources.

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“…In reference [14] down-going tau-neutrino events are also investigated. According to the estimated neutrino flux coming from Active Galactic Nuclei [23,24], Gamma Ray Bursts [25], Topological Defects [24,26], and Cosmogenic Neutrinos [27,28] as well as to the neutrino cross section extrapolated to ultra-high energies [29], it is expected a number of tauneutrino events in Auger approximately of the order of between 0.1 and 1 event per year, with energies around 1 EeV.…”

Section: Tau-neutrinos Interacting In the Atmospherementioning

confidence: 99%

New analyses of double-bang events in the atmosphere

Moura¹,

Guzzo²

2008

Braz. J. Phys.

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We use CORSIKA+Herwig simulation code to produce ultra-high energy neutrino interactions in the atmosphere. Our aim is to reproduce extensive air showers originated by extragalactic tau-neutrinos. For charged current tau-neutrino interactions in the atmosphere, beside the air shower originated from the neutrino interaction, it is expected that a tau is created and may decay before reaching the ground. That phenomenon makes possible the generation of two related extensive air showers, the so called Double-Bang event. We make an analysis of the main characteristics of Double-Bang events in the atmosphere for mean values of the parameters involved in such phenomenon, like the inelasticity and tau decay length. We discuss what may happen for the "out of the average" cases and conclude that it may be possible to observe this kind of event in ultra-high energy cosmic ray observatories such as Pierre Auger or Telescope Array.

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Ultrahigh-energy neutrino interactions

Cited by 582 publications

References 106 publications

Long-lived staus from cosmic rays

Long-lived staus from cosmic rays

The Glashow resonance at IceCube: signatures, event rates andppvs.pγ interactions

New analyses of double-bang events in the atmosphere

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