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10 17 eV decade

This paper examines the model dependence of the composition in the transition between the galactic and extragalactic cosmic ray components. It explores various models and subtracts the observed data to analyze and predict the transition energy. The results suggest a transition energy range of 10^16.5 to 10^17.5 eV, with a composition change signature. The study emphasizes the importance of energy resolution and recommends further investigations using HiRes, KASCADE-Grande, IceCube/IceTop, TALE, and Amiga/HEAT at Auger.

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10 17 eV decade

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  1. 1017 eV decade Breakout summary Tom Gaisser

  2. Alternatives for transition to E.G. Allard, Olinto, Parizot, astro-ph/0703633

  3. Model dependence of composition in galactic-extragalactic transition • Model extragalactic component • Subtract from observed • to get galactic component Allard, Olinto, Parizot, astro-ph/0703633 proton model mixed model Tom Gaisser

  4. Berezhko & Völk • Model galactic component • Subtract from observed • to get extragalactic Transition predicted: 1016.5 to 1017.5 eV arXiv:0704.1715v1 [astro-ph] Tom Gaisser

  5. HiRes new composition result: transition occurs before ankle 0.3 EeV G. Archbold, P. Sokolsky, et al., Proc. 28th ICRC, Tsukuba, 2003 Depth of Maximum • Early transition favored • HiRes prototype + CASA/MIA • HiRes (E > 1018) Stereo Tom Gaisser

  6. From heavy toward protons Composition from density of muonsρµ(600) vs. E0 (Akeno, AGASA) Calculations by Bruce Dawson with MoccaSibyll Tom Gaisser

  7. KASCADE-Grande : first analyses muon density investigations KASCADE-Grande preliminary T. Pierog (EPOS) MIA Tom Gaisser

  8. Cross section summary M BlockNote: old data are rescaled

  9. Interaction models • QGSjet01 • SIBYLL • QGSjet02 • EPOS Ralph Engel Tom Gaisser

  10. Tom Gaisser

  11. Hard p0 production of EPOS readily detectable in LHCf

  12. Attribute to NN production in EPOS More m in EAS with EPOS

  13. Xmax more stable Tom Gaisser

  14. Summary comments • Two very different models of transition • 1017 to 1018 -or- 1018 to 1019 eV • Strong composition change signature • HiRes favors low-energy transition • Model dependence a problem • Good energy resolution important • KASCADE-Grande, IceCube/IceTop, TALE, Amiga/HEAT at Auger Tom Gaisser

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