-
4
-
-
33744674909
-
-
AMS Collaboration, Phys. Lett. B 490, 27 (2000).
-
(2000)
Phys. Lett. B
, vol.490
, pp. 27
-
-
-
6
-
-
85038311818
-
-
M. Circella et al., in Proceedings of the 27th International Cosmic-Ray Conference, Hamburg, Report No. HE260, 2001.
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M. Circella et al., in Proceedings of the 27th International Cosmic-Ray Conference, Hamburg, Report No. HE260, 2001.
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-
-
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10
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85038282145
-
-
T. Tamura et al., in Proceeding of the 26th International Cosmic-Ray Conference, Utah, Report No. OG4. 1. 06, 1999.
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T. Tamura et al., in Proceeding of the 26th International Cosmic-Ray Conference, Utah, Report No. OG4. 1. 06, 1999.
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-
-
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11
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85038301968
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-
We note electron showers of 10 GeV are normally simulated by (Formula presented) protons when the latter start to cascade at a shallow depth of the detector.
-
We note electron showers of 10 GeV are normally simulated by (Formula presented) protons when the latter start to cascade at a shallow depth of the detector.
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-
-
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12
-
-
85038321485
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-
If we do not impose the trigger condition, the gamma-ray case shows a small difference from the electron case.
-
If we do not impose the trigger condition, the gamma-ray case shows a small difference from the electron case.
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-
-
-
13
-
-
85038292876
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S. Torii et al., in Composition and Origin of Cosmic Rays, edited by Y. Suzuki, M. Nakahata, M. Shiozawa, and K. Kaneyuki (Universal Academy Press, Tokyo, 2000), p. 35.
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S. Torii et al., in Composition and Origin of Cosmic Rays, edited by Y. Suzuki, M. Nakahata, M. Shiozawa, and K. Kaneyuki (Universal Academy Press, Tokyo, 2000), p. 35.
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-
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14
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85038288745
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The chance coincidence probability of uncorrelated particles is negligibly small.
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The chance coincidence probability of uncorrelated particles is negligibly small.
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-
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15
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85038277321
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URL http://cosmos.n.kanagawa-u.ac.jp/∼kasahara/ ResearchHome/cosmosHome/index.html
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URL http://cosmos.n.kanagawa-u.ac.jp/∼kasahara/ ResearchHome/cosmosHome/index.html
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17
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-
85038281116
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-
It is used at energies greater than 4.5 GeV. At lower energies, nucrin/hadrin
-
It is used at energies greater than 4.5 GeV. At lower energies, nucrin/hadrin 18 is used.
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-
-
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19
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-
33751196754
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M. Honda, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D 52, 4985 (1995).
-
(1995)
Phys. Rev. D
, vol.52
, pp. 4985
-
-
Honda, M.1
Kajita, T.2
Kasahara, K.3
Midorikawa, S.4
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21
-
-
85038336667
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-
It is used at energies greater than 10 GeV. At lower energies, the model is the same as FRITIOF1.6.
-
It is used at energies greater than 10 GeV. At lower energies, the model is the same as FRITIOF1.6.
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-
-
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22
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85038328249
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Proceeding of “Monte Carlo 2000,” Lisbon, Portugal, Vol. 71, p. 23.
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S. Roesler, R. Engel, and J. Ranft, Report No. SLAC-PUB-8740, hep-ph/0012252;Proceeding of “Monte Carlo 2000,” Lisbon, Portugal, Vol. 71, p. 23.
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-
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Roesler, S.1
Engel, R.2
Ranft, J.3
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23
-
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85038323677
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Compilation by J. A. Simpson, in Composition and Origin of Cosmic Rays, edited by M. M. Shapiro (Reidel, Dordrecht, 1982), p. 1.
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Compilation by J. A. Simpson, in Composition and Origin of Cosmic Rays, edited by M. M. Shapiro (Reidel, Dordrecht, 1982), p. 1.
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24
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33744711883
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AMS Collaboration, Phys. Lett. B 484, 10 (2000).
-
(2000)
Phys. Lett. B
, vol.484
, pp. 10
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-
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27
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85038329167
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-
Figure 4-1 of Ref.
-
Figure 4-1 of Ref. 26 is the integral vertical flux which includes electrons. This was converted to the differential flux of gamma-rays by one of the authors (J.N.). Conversion by cascade theory is accurate at high energies; (Formula presented) coincides with the present simulation data. The energy determination method at that time is the same as the one used in primary electron observation with emulsion chambers and the method has been confirmed by an FNAL calibration experiment 28.
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-
-
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29
-
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85038315622
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-
These are not based on particular observational data. However, the proton flux at around 10 TeV is close to the Runjob result
-
These are not based on particular observational data. However, the proton flux at around 10 TeV is close to the Runjob result 30 and (Formula presented) higher than the fitted curve (dashed line in Fig. 6) of Ref. 2. As to the He, the flux is (Formula presented) lower than a fitted curve (dashed line in Fig. 66) of the same reference, but higher by a factor of (Formula presented) (at 10 TeV) and (Formula presented) (at 100 TeV) than another fitted curve (dotted line).
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-
-
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31
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-
85038332732
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-
T. Sanuki (private communication).
-
T. Sanuki (private communication).
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-
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32
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85038274098
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M. Honda et al., in Proceeding of the 27th International Cosmic-Ray Conference, Hamburg, 2001, Vol. 3, p. 1162.
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M. Honda et al., in Proceeding of the 27th International Cosmic-Ray Conference, Hamburg, 2001, Vol. 3, p. 1162.
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34
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85038330234
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R. Engel et al., in Proceeding of the 27th International Cosmic-Ray Conference
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R. Engel et al., in Proceeding of the 27th International Cosmic-Ray Conference 30, Vol. 4, p. 1381.
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