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

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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

- 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.

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)

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

- 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.

- 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 “

- 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 )

- 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

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

EμCherenkov Light(t)

N=N+1

- 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))

The first prediction on the characteristics of the LPM shower

Nuovo Cimento 48A, 509 (1978)

E0/Em=103

E0/Em=103

BH

BH

LPM

LPM

The first prediction on the multi-peak structure of the LPM shower.

E0=1017 eV Emin=109 eV

The same LPM shower with different threshold energies.

Eth=109 eV

Eth=1012 eV

Eth=1014 eV

The LPM shower with deep crevasse.

E0=1017 eV

Em=109 eV

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

Fractional dissipated energies of the LPM shower in water.

4848 cu = 1700 meters

- 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