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Akeo Misaki Research Institute For Science and engineering, Waseda University, Tokyo, Japan

On the Characteristics of the Neutrino Events in (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation. Akeo Misaki Research Institute For Science and engineering, Waseda University, Tokyo, Japan. Invitation to a point in dispute.

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Akeo Misaki Research Institute For Science and engineering, Waseda University, Tokyo, Japan

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  1. On the Characteristics of the Neutrino Events in (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation Akeo Misaki Research Institute For Science and engineering, Waseda University, Tokyo, Japan

  2. Invitation to a point in dispute • The Fundamental parameters in (Ultra-)High Energy Astrophysics are: 1.Reliable Estimation of the Energies of the Neutrino Events 2. Reliable Estimation of the Incident Direction of the Neutrino Events To invite the participants to a point dispute, let us start from CONCLUSION, not INTRODUCTION.

  3. Conclusion 1 1. Muon Neutrino Events: Inevitably Partially Contained Events One could not even estimate the energies of the muons from muon neutrino events (! ?) 2. Electron Neutrino Events: Usually, Fully Contained Events. Inevitably, Partially Contained Events in Ultra-High Energies (LPM shower)

  4. Conclusion 2 • COMPUTER NUMERICAL EXPERIMENTS • should be carried out simultaneously together with the REAL XPERIMENTS CONCERNED, not in the usual sense of Monte Carlo Simulation.

  5. Range Fluctuation of (Ultra)-High Energy Muons • The Muon Range with Definite Energy is governed by the stochastic characters of the direct electron pair production, remsstrahlung and nuclear interaction which are also the origins of the accompanied electron showers.

  6. Range Fluctuation of (Ultra-) High Energy Muon

  7. The Image of (Ultra-)High Energy Muon • Muons from Muon Neutrino Events should be recognized as an aggregate of electron cascade showers with different starting points and different primary energies. • “Electron clouds” are twined around such the muon. • Namely, the muon could not be imaged as “Single or Naked Muon “

  8. Is the Muon Itself the Dominant Source for the Cherenkov Light ? • For the question, it enough to examine the track lengths concerned, because the Cherenkov light production is proportional to the corresponding track length. • Ratio= track lengths of electrons from the accompanied showers/(track lengths of electrons from the accompanied showers + track length of the muon )

  9. The transition curves for the integral of the track lengths from the muon as whole

  10. Cherenkov Light from the Mother Muon and Her Daughters Electron Shower • Accompanied electron showers are produced from the direct electron pair production, beremsstrahlung and nuclear interaction due to muon. • These electron showers are exactly simulated in one-dimensional treatment . • The electron segments in the simulated electron showers produced corresponding Cherenkov light

  11. The Exactly Simulated Energy Losses of a Muon with 100 TeVas the Function of the traversed depth

  12. The Exactly Simulated Energy losses of a Muon with 1 PeV as the function of the traveresed distance

  13. Five Examples of Transition Curves for the Cherrenkov Light

  14. Cherenkov Photon Number Distribution at 1000m

  15. Cherenkov Light vs. Muon Energy A production Spectrum for Muon Nμ(Eμ)dEμ∝ Eμ－(γ+1) dEμ N=1 For givenγ No N≦Nmax Yes Random sampling ofEμ from Eμ－(γ+1) dEμ Eμ EμCherenkov Light(t) N=N+1

  16. Energy Estimation of Muon for given Cherenkov Light1

  17. Energy Estimation of Muon for Given Cherenkov Light 2

  18. The LPM showersas Partially Contained Events • The Characteristics of the LPM showers: • [1] The Average behavior of the LPM showers is quite different from that of BH (Bethe-Heitler) Showers ( Konishi,Misaki and Fujimaki, Nuovo Cimento,(1978)) • [2] TheIndividual Behavior of the LPM shower is quite different from that of the Averaged LPM shower ( Konishi,Adachi,Takahashi and Misaki, J.Phys.G, (1991))

  19. The first prediction on the characteristics of the LPM shower Nuovo Cimento 48A, 509 (1978)

  20. First Example of the LPM shower E0/Em=103 E0/Em=103 BH BH LPM LPM

  21. First Example of Multi-Peak The first prediction on the multi-peak structure of the LPM shower.

  22. Multi-peak threshold E0=1017 eV Emin=109 eV The same LPM shower with different threshold energies. Eth=109 eV Eth=1012 eV Eth=1014 eV

  23. Multi-Peal Ctrevasse The LPM shower with deep crevasse. E0=1017 eV Em=109 eV

  24. The first Description The first description on the average behavior of the LPM shower in water.

  25. Fractional Dissipated Fractional dissipated energies of the LPM shower in water. 4848 cu = 1700 meters

  26. LPM shower electron number E0=10^15 eV

  27. LPM shower track length E0=10^15 eV

  28. LPM shower electron number E0=10^18 eV

  29. LPM shower track length E0=10^18 eV

  30. LPM shower electron number E0=10^21 eV

  31. LPM shower track length E0=10^21 eV

  32. Final Conclusion • At the early stage of the REAL XPERIMENTS, COMPUTER NUMRERICAL XPERIMENT should be being carried out with parallel them, collaborating with them closely. • In the presence of the Computer numerical experiment, one need not the transformation from the Cherenkov light to the Muon Energy

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