메뉴 건너뛰기




Volumn 66, Issue 5, 2002, Pages

Atmospheric gamma-ray observation with the BETS detector for calibrating atmospheric neutrino flux calculations

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; CALCULATION; COSMOS; GAMMA RADIATION; MODEL; MOLECULAR INTERACTION; OSCILLATION; RADIATION DETECTION; THICKNESS;

EID: 18344405595     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.66.052004     Document Type: Article
Times cited : (18)

References (35)
  • 4
    • 33744674909 scopus 로고    scopus 로고
    • AMS Collaboration, Phys. Lett. B 490, 27 (2000).
    • (2000) Phys. Lett. B , vol.490 , pp. 27
  • 6
    • 85038311818 scopus 로고    scopus 로고
    • M. Circella et al., in Proceedings of the 27th International Cosmic-Ray Conference, Hamburg, Report No. HE260, 2001.
    • M. Circella et al., in Proceedings of the 27th International Cosmic-Ray Conference, Hamburg, Report No. HE260, 2001.
  • 10
    • 85038282145 scopus 로고    scopus 로고
    • T. Tamura et al., in Proceeding of the 26th International Cosmic-Ray Conference, Utah, Report No. OG4. 1. 06, 1999.
    • T. Tamura et al., in Proceeding of the 26th International Cosmic-Ray Conference, Utah, Report No. OG4. 1. 06, 1999.
  • 11
    • 85038301968 scopus 로고    scopus 로고
    • 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.
  • 12
    • 85038321485 scopus 로고    scopus 로고
    • 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.
  • 13
    • 85038292876 scopus 로고    scopus 로고
    • 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.
    • 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.
  • 14
    • 85038288745 scopus 로고    scopus 로고
    • The chance coincidence probability of uncorrelated particles is negligibly small.
    • The chance coincidence probability of uncorrelated particles is negligibly small.
  • 15
    • 85038277321 scopus 로고    scopus 로고
    • URL http://cosmos.n.kanagawa-u.ac.jp/∼kasahara/ ResearchHome/cosmosHome/index.html
    • URL http://cosmos.n.kanagawa-u.ac.jp/∼kasahara/ ResearchHome/cosmosHome/index.html
  • 17
    • 85038281116 scopus 로고    scopus 로고
    • 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.
  • 21
    • 85038336667 scopus 로고    scopus 로고
    • 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.
  • 22
    • 85038328249 scopus 로고    scopus 로고
    • Proceeding of “Monte Carlo 2000,” Lisbon, Portugal, Vol. 71, p. 23.
    • 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.
    • Roesler, S.1    Engel, R.2    Ranft, J.3
  • 23
    • 85038323677 scopus 로고    scopus 로고
    • Compilation by J. A. Simpson, in Composition and Origin of Cosmic Rays, edited by M. M. Shapiro (Reidel, Dordrecht, 1982), p. 1.
    • Compilation by J. A. Simpson, in Composition and Origin of Cosmic Rays, edited by M. M. Shapiro (Reidel, Dordrecht, 1982), p. 1.
  • 24
    • 33744711883 scopus 로고    scopus 로고
    • AMS Collaboration, Phys. Lett. B 484, 10 (2000).
    • (2000) Phys. Lett. B , vol.484 , pp. 10
  • 27
    • 85038329167 scopus 로고    scopus 로고
    • 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.
  • 29
    • 85038315622 scopus 로고    scopus 로고
    • 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).
  • 31
    • 85038332732 scopus 로고    scopus 로고
    • T. Sanuki (private communication).
    • T. Sanuki (private communication).
  • 32
    • 85038274098 scopus 로고    scopus 로고
    • M. Honda et al., in Proceeding of the 27th International Cosmic-Ray Conference, Hamburg, 2001, Vol. 3, p. 1162.
    • M. Honda et al., in Proceeding of the 27th International Cosmic-Ray Conference, Hamburg, 2001, Vol. 3, p. 1162.
  • 34
    • 85038330234 scopus 로고    scopus 로고
    • R. Engel et al., in Proceeding of the 27th International Cosmic-Ray Conference
    • R. Engel et al., in Proceeding of the 27th International Cosmic-Ray Conference 30, Vol. 4, p. 1381.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.