Neutrino interactions at ultrahigh energies

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

doi:10.1103/physrevd.58.093009

Cited by 578 publications

(793 citation statements)

References 60 publications

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“…This because of proliferous, penetrating nature of the muon. Due to the neutrino flux paucity and its low cross-section most of the detector are large as Super Kamiokande or larger volumes as AMANDA, Baikal or Antares ones, looking to km 3 future size [20]. Because most of cosmic rays are converting into atmospheric muon secondaries, the muon dawn ward directions are polluted by atmospheric noises.…”

Section: Past Neutrino Telescope Undergroundmentioning

confidence: 99%

“…The opacity is related to the electroweak cross-section dependence on incoming neutrino energy with matter [20] and, of course, on the planet size and composition. Smallest radius allows greater neutrino energy: for the Earth diameter the neutrino cut-off is about 4·10 13 eV for ν µ and 10 15 eV for ν τ (because of their marginal regeneration and pile up by higher energies neutrinos toward PeV band).…”

Section: The Titan Role In Uptaus Showeringmentioning

confidence: 99%

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UHE Cosmic Rays and Neutrinos Showering on Planet Edges

Fargion

Oliva

Lanciano

2007

Nuclear Physics B - Proceedings Supplements

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Ultra High Energy (UHE) Cosmic Rays, UHECR, may graze high altitude atmosphere leading to horizontal upward air-showers. Also PeVs electron antineutrino hitting electron in atmosphere may air-shower at W boson resonant mass. On the other side ultra high energy muon and electron neutrinos may also lead, by UHE neutrinos mass state mixing, to the rise of a corresponding UHE Tau neutrino flavor; the consequent UHE tau neutrinos, via charge current interactions in matter, may create UHE taus at horizons (Earth skimming neutrinos or Hor-taus) whose escape in atmosphere and whose consequent decay in flight, may be later amplified by upward showering on terrestrial, planetary atmospheres. Indeed because of the finite terrestrial radius, its thin atmosphere size its dense crust, the UHE tau cannot extend much more than 360 kilometers in air, corresponding to an energy of about 7.2 EeV, near but below GZK cut-off ones; on the contrary Jupiter (or even Saturn) may offer a wider, less dense and thicker gaseous layer at the horizons where Tau may loose little energy, travel longer before decay and rise and shower at 4-6 10^{19} eV or ZeV extreme energy. Titan atmosphere may open a rare window of opportunity for Up-ward Taus at PeVs. Also solar atmosphere may play a role, but unfortunately tau-showers secondaries maybe are too noisy to be disentangled, while Jupiter atmosphere, or better, Saturn one, may offer a clearer imprint for GZK (and higher Z-Burst) Tau showering, well below the horizons edges.Comment: 8 pages, 16 Figures, CRIS 200

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Section: Past Neutrino Telescope Undergroundmentioning

confidence: 99%

Section: The Titan Role In Uptaus Showeringmentioning

confidence: 99%

UHE Cosmic Rays and Neutrinos Showering on Planet Edges

Fargion

Oliva

Lanciano

2007

Nuclear Physics B - Proceedings Supplements

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“…When instead the showers are produced by deep inelastic neutrino scattering off target nucleons, the fraction of the total energy which produces the hadronic showers is, on average, E s = 0.25E P [23].…”

Section: Aperture For Cosmic Ray and Neutrino Events At Gmrtmentioning

confidence: 99%

“…The radio waves are also absorbed in the regolith, which we take to have a frequency dependent attenuation length λ r = 9/(ν/GHz) m [22]. This means the attenuation length of radio waves is always much smaller than the mean free path of the neutrinos, conveniently parameterized as λ ν = 670(1 EeV/E ν ) 0.363 km using the cross sections of [23]. As can be seen from this expression, the mean free path for an UHE neutrino is not sufficient to escape the Moon.…”

Section: Aperture For Cosmic Ray and Neutrino Events At Gmrtmentioning

confidence: 99%

Prospects for the Giant Metrewave Radio Telescope to observe radio waves from ultra high energy particles interacting with the Moon

Panda

Mohanty

Janardhan

et al. 2007

J. Cosmol. Astropart. Phys.

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Ultra high energy (UHE) particles of cosmic origin impact the lunar regolith and produce radio signals through Askaryan effect, signals that can be detected by Earth based radio telescopes. We calculate the expected sensitivity for observation of such events at the Giant Metrewave Radio Telescope (GMRT), both for UHE cosmic rays (CR) and UHE neutrino interactions. We find that for 30 days of observation time a significant number of detectable events is expected above 10 20 eV for UHECR or neutrino fluxes close to the current limits. Null detection over a period of 30 days will lower the experimental bounds by a magnitude competitive to both present and future experiments at the very highest energies.

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“…which is the SM extrapolation for the neutrinos plus antineutrinos and nuclei cross section in charged current interactions , which have 10% accuracy within the energy range 10 −2 < E(EeV) < 10 3 when compared with the results of the CTEQ4-DIS parton distributions [20].…”

Section: Event Ratementioning

confidence: 99%

Detection of ultra high-energy tau-neutrinos with fluorescence detectors

Moura¹,

Guzzo²

2007

Braz. J. Phys.

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We calculate the possible number of Extensive Air Showers originated by tau neutrinos in Fluorescence Detectors like the ones of the Pierre Auger Observatory. We consider models of production of electron and muon neutrinos in extra galactic objects and Topological Defects, as well as the possibility of neutrino flavor change in the propagation of the neutrinos between the source and the Earth. The neutrino cross section was calculated by the extrapolation of the standard model parton distribution functions until energies of the order of 10 21 eV. However, due to uncertainties in the extrapolation for energies higher than 10 12 eV the results are not robust. We conclude that, depending on the relation between flux and cross section, there is a strict range of energy for the tau neutrinos to generate double extensive air showers detectable in Fluorescence Detectors. The tau neutrino energy must be approximately 10 18 eV and the event rate can vary some orders of magnitude around one event per year, depending on the flux-cross section relation and detector characteristics.

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Neutrino interactions at ultrahigh energies

Cited by 578 publications

References 60 publications

UHE Cosmic Rays and Neutrinos Showering on Planet Edges

UHE Cosmic Rays and Neutrinos Showering on Planet Edges

Prospects for the Giant Metrewave Radio Telescope to observe radio waves from ultra high energy particles interacting with the Moon

Detection of ultra high-energy tau-neutrinos with fluorescence detectors

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