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EHE Cosmic Rays, EHE Neutrinos and GeV- TeV Gamma rays

EHE Cosmic Rays, EHE Neutrinos and GeV- TeV Gamma rays. David Kieda University of Utah Department of Physics. Outline. GZK energy Cosmic Ray Measurements GZK energy Cosmic Ray Origin EHE neutrino production EHE neutrino fluxes Conclusion. UHE/EHE Cosmic Ray Astrophysics.

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EHE Cosmic Rays, EHE Neutrinos and GeV- TeV Gamma rays

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  1. EHE Cosmic Rays, EHE Neutrinos and GeV- TeV Gamma rays David Kieda University of Utah Department of Physics

  2. Outline • GZK energy Cosmic Ray Measurements • GZK energy Cosmic Ray Origin • EHE neutrino production • EHE neutrino fluxes • Conclusion ANITA Meeting UCI

  3. UHE/EHE Cosmic Ray Astrophysics HiRes Fly’s Eye (2002) ANITA Meeting UCI

  4. EHE Cosmic Ray Astrophysics Fly’s Eye Detector (Dugway, Utah) Hires Fly’s Eye Detector (Dugway, Utah) ANITA Meeting UCI

  5. EHE Cosmic Ray Astrophysics GZK cutoff: (d>20 Mpc) Greisen PRL 16, 748 (1966) Zatsepin & Kuzmin JETP Lett 4, 78 (1966) 320 EeV Cosmic Ray: Energy beyond GZK cutoff (D. Bird et al Ap. J 441, 144 (1995)) ANITA Meeting UCI

  6. EHE Cosmic Ray Spectrum HiRes Fly’s Eye (2002) ANITA Meeting UCI

  7. EHE Cosmic Ray Spectrum AGASA Array (2002) ANITA Meeting UCI

  8. EHE Cosmic Ray Spectrum Discrepancy due to differences energy scale factors (within quoted systematics)? A simple energy rescale looks promising, But….. Aertures are energy dependent (especially for HiRes & Fly’s Eye) Bachall & Waxman (2002) ANITA Meeting UCI

  9. EHE Cosmic Ray Arrival Directions Large Scale Anisotropy: Probe correlation with anisotropy of local Galactic population (SuperGalactic Plane) or Galactic Center, Galactic Plane. >AGN, starburst, magentar, GRB populations correlated with luminous mass >Dark Matter Halo: Annihilation, Z-burst of relic massive neutrinos Small Scale Anisotropy: Event clustering with < 10 degree separation. Point source searches. Competition between increasing particle rigidity and decreasing statistic>Narrow energy window? Cosmic Ray Akeno (2000). Clustering random chance probabilty ~1% In conflict with HiRes experiment (similar exposure) Hamburg 2001). ANITA Meeting UCI

  10. EHE Cosmic Ray SourcesBottom-Up ANITA Meeting UCI

  11. EHE Cosmic Ray PropagationEffects 1) Quantum Gravity Lorentz violation eliminates GZK (Gonzales-Mestres 1999, 2000) *Reduced interaction cross section (smaller final product phase space) *Reduced Lorentz boosted energy of CMB -> Probe with time delay of TeV Gamma rays from AGN 2) Z-Burst Models: High Energy Neutrino interacts with heavy relic neutrino in Galactic DM halo (But isn’t this just making thing worse?) ANITA Meeting UCI

  12. EHE Cosmic Ray PropagationEffects If CR are indeed extragalactic, and if GZK cutoff does exist, pion decay leads to guaranteed neutrino flux. Adapted from C. Spiering (2002). ANITA Meeting UCI

  13. EHE Cosmic Ray SourcesBottom-Up AGN with Pair production creating dip at 10 EeV V. Berezinsky et al (2002) ANITA Meeting UCI

  14. EHE Cosmic Ray SourcesBottom-Up Nearby Magnetars population (< 50 Mpc) with PetaGauss B fields yields dip Arons astro-ph/0208444 ANITA Meeting UCI

  15. EHE Cosmic Ray SourcesTop-Down Typical Topological defect fragmentation: Production of gammas, e+/e-, neutrinos with fluxes substantially greater than the cosmic rays (O. Kalashev et al 2002) ANITA Meeting UCI

  16. EHE Neutrinos • Top-Down Models vs. Bottom up give strongly different predictions for Neutrino flux • Absolute neutrino flux constrained by gamma/neutrino production ratio (GeV/TeV gamma measurements) • Absolute neutrino flux constrained by absolute cosmic ray flux (Bachall & Waxman bound, Mannheim, Protheroe & Rachen bound) Some wiggle room if sources are opaque to gammas/cosmic rays and/or large distances to CR sources MAGIC, 1 tel., 2003 VERITAS, 2005 4 tel. 2007 7 tel. ANITA 2005 flight GLAST 2005 flight ANITA Meeting UCI

  17. EHE Neutrinos Production: • Direct production in Top-Down Models (Topologcal defect decay, super-heavy dark matter annihilation, super-heavy X particle decay) Peak Energy ~100 EeV ANITA Meeting UCI

  18. EHE Neutrinos Production: • Direct production in Top-Down Models Z-burst (Gelmaini, Cline, others) Peak Energy > 100 EeV ANITA Meeting UCI

  19. EHE Neutrinos Production: • Secondary interactions of CR &  production/decay near acceleration region at EHE CR source (AGN, GRB) Peak energy ~ 10 PeV (Stecker and Salamon 1996) ANITA Meeting UCI

  20. EHE Cosmic Ray Backgroundfor Radio Cherenkov Measurements? Shock Wave ANITA Meeting UCI

  21. EHE Neutrino Observations ANITA pushes EeV neutrino limits >Well below diffuse gamma/MPR bounds >Approaches W&B bond C. Spiering (2002). ANITA Meeting UCI

  22. Conclusions Super GZK Cosmic rays Exist. Rate, energy spectrum, isotropy statistically limited Difficult to separate Top-Down vs. Bottom up models in cosmic ray properties TeV Gamma, BW & MPR bounds do not exclude a strongly peaked  flux above 100 EeV. GZK+Universal EHE CR production yields predictable 10-100 EeV  flux Absence of GZK  production probably implies GQ Lorentz violation Confluence of next generation TeV gamma ray, high energy neutrino & high energy cosmic ray provide strong constraints. Radio observations by ANITA play a key role in the next 5-10 years. Shock Wave ANITA Meeting UCI

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