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GZK EHE n detection

This study explores the GZK mechanism and the detection of extremely high-energy (EHE) neutrinos using the IceCube facility. It discusses EHE neutrino propagation in the Earth, expected event rates, and interactions with atmospheric backgrounds. The research highlights the significance of neutrino oscillations and presents predictions for the intensity of GZK neutrinos at various depths. It concludes that IceCube can effectively detect GZK neutrinos, estimating a detection rate of 0.2 to 40 events per year, surpassing atmospheric noise.

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GZK EHE n detection

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  1. TAUP 2003 GZK EHEn detection • What is the GZK mechanism? • EHE n/m/t Propagation in the Earth • Expected intensities at the IceCube depth • Atmospheric m – background • Event rate

  2. GZK Neutrino Production 0.6 x 10-27 cm2 2.725 K 411 photons / cm3 π ν ＋ ＋ γ μ ＋ ν e p γ p n E = 10 20 eV Conventional Mechanism of EHE neutrinos!! E 0.8 x 10 20 eV ~

  3. Note: The oscillations convert ne, nm to ne,nm, nt Yoshida and Teshima 1993 Yoshida, Dai, Jui, Sommers 1997 TAUP 2003

  4. t/m propagation in Earth TAUP 2003

  5. Products ne nm nt m t p e/g ne Weak Weak nm Weak Weak nt Weak Weak Incoming e/g Cascades Decay Weak Pair/decay Bremss Decay m Pair Pair PhotoNucl. DecayPair Decay Pair Bremss Decay Decay Weak t Pair PhotoNucl. p Cascades

  6. Suppression By t decay Muon(Neutrinos) from nm nt Tau(Neutrinos) from nm nt Nadir Angle TAUP 2003

  7. ν Downward lepton γ γ ± π + + e e － － e e １．４ｋｍ １ｋｍ Ice γ ν lepton １ｋｍ Rock ν Upward

  8. Atmospheric muon! – a major backgrond But so steep spectrum Upward-going Downward going!! TAUP 2003

  9. 11000m 2800 m 1400 m Down-going events dominates… Atmospheric m is strongly attenuated… Up Down TAUP 2003

  10. Flux as a function of energy deposit in km3 • dE/dX~bE DE~DXbE

  11. Up Down TAUP 2003

  12. Intensity of EHE m and t [cm-2 sec-1] TAUP 2003

  13. How EHE events look like Eµ=10 TeV ≈ 90 hits Eµ=6 PeV ≈ 1000 hits The typical light cylinder generated by a muon of 100 GeV is 20 m, 1PeV 400 m, 1EeV it is about 600 to 700 m.

  14. Conclusion t/m appeared in 10 PeV- EeV are our prime target on GZK n detection. 1/100-1/500 of primary n intensity! Downwardt and m make main contributions in PeV -EeV Energy Estimation would be a key for the bg reduction Because atmospheric m spectrum ~ E-3.7 TAUP 2003 IceCube has great capability for TeV-PeV n-induced muons taking advantage of long range in the clear ice. For EHE n like the GZK…. GZK n is DETECTABLE by IceCube 0.2-40 events/year (BG 0.05 events/year)

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