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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. Invitation to a point in dispute.

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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


Invitation to a point in dispute
Invitation to (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimationa 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.


Conclusion 1
Conclusion 1 (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation

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)


Conclusion 2
Conclusion 2 (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation

  • COMPUTER NUMERICAL EXPERIMENTS

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


Range fluctuation of ultra high energy muons
Range Fluctuation (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation 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.


Range fluctuation of ultra high energy muon
Range Fluctuation of (Ultra-) High Energy Muon (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation


The image of ultra high energy muon
The Image of (Ultra-)High Energy Muon (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimation

  • 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 “


Is the muon itself the dominant source for the cherenkov light
Is the Muon Itself (Ultra-)High Energy Astrophysics Experiments from the view point of Energy Estimationthe 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 )



Cherenkov light from the mother muon and her daughters electron shower
Cherenkov Light from from the muon as wholethe 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



The exactly simulated energy losses of a muon with 1 pev as the function of the traveresed distance
The Exactly Simulated Energy losses of a Muon with 1 PeV as the function of the traveresed distance


Five examples of transition curves for the cherrenkov light
Five Examples of Transition Curves for the Cherrenkov Light the function of the traveresed distance


Cherenkov photon number distribution at 1000m
Cherenkov Photon Number Distribution at 1000m the function of the traveresed distance


Cherenkov light vs muon energy
Cherenkov Light vs. Muon Energy the function of the traveresed distance

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Cherenkov Light(t)

N=N+1


Energy estimation of muon for given cherenkov light 1
Energy Estimation of Muon for given Cherenkov Light the function of the traveresed distance1


Energy estimation of muon for given cherenkov light 2
Energy Estimation of Muon for Given Cherenkov Light 2 the function of the traveresed distance


The lpm showers as partially contained events
The LPM showers the function of the traveresed distanceas 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))


The first prediction on the characteristics of the lpm shower

The first prediction the function of the traveresed distance on the characteristics of the LPM shower

Nuovo Cimento 48A, 509 (1978)


First example of the lpm shower
First Example of the LPM shower the function of the traveresed distance

E0/Em=103

E0/Em=103

BH

BH

LPM

LPM


First example of multi peak
First Example of Multi-Peak the function of the traveresed distance

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


Multi peak threshold
Multi-peak threshold the function of the traveresed distance

E0=1017 eV Emin=109 eV

The same LPM shower with different threshold energies.

Eth=109 eV

Eth=1012 eV

Eth=1014 eV


Multi peal ctrevasse
Multi-Peal Ctrevasse the function of the traveresed distance

The LPM shower with deep crevasse.

E0=1017 eV

Em=109 eV


The first description
The first Description the function of the traveresed distance

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


Fractional dissipated
Fractional Dissipated the function of the traveresed distance

Fractional dissipated energies of the LPM shower in water.

4848 cu = 1700 meters


Lpm shower electron number e0 10 15 ev
LPM shower electron number E0=10^15 eV the function of the traveresed distance


Lpm shower track length e0 10 15 ev
LPM shower track length E0=10^15 eV the function of the traveresed distance


Lpm shower electron number e0 10 18 ev
LPM shower electron number E0=10^18 eV the function of the traveresed distance


Lpm shower track length e0 10 18 ev
LPM shower track length E0=10^18 eV the function of the traveresed distance


Lpm shower electron number e0 10 21 ev
LPM shower electron number E0=10^21 eV the function of the traveresed distance


Lpm shower track length e0 10 21 ev
LPM shower track length E0=10^21 eV the function of the traveresed distance


Final conclusion
Final Conclusion the function of the traveresed distance

  • 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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