Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala

J. R. Ren, H. H. Kuang, A. X. Huo, S. L. Lu, S. Su, Y. X. Wang, C. R. Wang, M. He, N. J. Zhang, P. Y. Cao, J. Y. Li, S. Z. Wang, G. Z. Bai, Z. H. Liu, G. J. Li, G. X. Gang, W. D. Zhou, R. D. He, M. Amenomori, H. NanjoN. Hotta, I. Ohta, K. Mizutani, K. Kasahara, T. Yuda, M. Shibata, T. Shirai, N. Tateyama, Shoji Torii, H. Sugimoto, K. Taira

Research output: Contribution to journal › Article

11 Citations (Scopus)

Abstract

We report on the results of the measurements of energy spectra of atmospheric cosmic rays in the energy around 10 TeV measured with emulsion chambers at Mt. Kanbala (5500 m above sea-level, atmospheric depth 520 g/cm2). The power indices of the integral spectra take the values of 2.00±0.08 for gamma-rays and 1.90±0.10 for hadrons, in the energy range from 5 TeV to 20 TeV. Their intensities are compatible with those expected from the primary cosmic rays containing fewer protons than in the lower energy region. The energy spectrum of family events is also discussed with reference to the composition of primary cosmic rays. It is concluded that the portion of protons in the primary cosmic rays gradually decreases in the energy range from 1013 eV to 1015 eV.

Original languageEnglish
Pages (from-to)43-60
Number of pages18
JournalIl Nuovo Cimento C
Volume10
Issue number1
DOIs
Publication statusPublished - 1987 Jan
Externally publishedYes

Fingerprint

primary cosmic rays
Cosmic rays
Emulsions
emulsions
cosmic rays
chambers
Chemical analysis
Protons
energy spectra
Hadrons
protons
energy
Sea level
sea level
Gamma rays
hadrons
gamma rays

Keywords

  • Cosmic rays

ASJC Scopus subject areas

  • Ocean Engineering
  • Mechanical Engineering
  • Electrical and Electronic Engineering
  • Control and Systems Engineering
  • Engineering (miscellaneous)
  • Nuclear Energy and Engineering
  • Computer Science Applications
  • Chemical Engineering(all)

Cite this

Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala. / Ren, J. R.; Kuang, H. H.; Huo, A. X.; Lu, S. L.; Su, S.; Wang, Y. X.; Wang, C. R.; He, M.; Zhang, N. J.; Cao, P. Y.; Li, J. Y.; Wang, S. Z.; Bai, G. Z.; Liu, Z. H.; Li, G. J.; Gang, G. X.; Zhou, W. D.; He, R. D.; Amenomori, M.; Nanjo, H.; Hotta, N.; Ohta, I.; Mizutani, K.; Kasahara, K.; Yuda, T.; Shibata, M.; Shirai, T.; Tateyama, N.; Torii, Shoji; Sugimoto, H.; Taira, K.

In: Il Nuovo Cimento C, Vol. 10, No. 1, 01.1987, p. 43-60.

Research output: Contribution to journal › Article

Ren, JR, Kuang, HH, Huo, AX, Lu, SL, Su, S, Wang, YX, Wang, CR, He, M, Zhang, NJ, Cao, PY, Li, JY, Wang, SZ, Bai, GZ, Liu, ZH, Li, GJ, Gang, GX, Zhou, WD, He, RD, Amenomori, M, Nanjo, H, Hotta, N, Ohta, I, Mizutani, K, Kasahara, K, Yuda, T, Shibata, M, Shirai, T, Tateyama, N, Torii, S, Sugimoto, H & Taira, K 1987, 'Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala', Il Nuovo Cimento C, vol. 10, no. 1, pp. 43-60. https://doi.org/10.1007/BF02508696
Ren JR, Kuang HH, Huo AX, Lu SL, Su S, Wang YX et al. Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala. Il Nuovo Cimento C. 1987 Jan;10(1):43-60. https://doi.org/10.1007/BF02508696
Ren, J. R. ; Kuang, H. H. ; Huo, A. X. ; Lu, S. L. ; Su, S. ; Wang, Y. X. ; Wang, C. R. ; He, M. ; Zhang, N. J. ; Cao, P. Y. ; Li, J. Y. ; Wang, S. Z. ; Bai, G. Z. ; Liu, Z. H. ; Li, G. J. ; Gang, G. X. ; Zhou, W. D. ; He, R. D. ; Amenomori, M. ; Nanjo, H. ; Hotta, N. ; Ohta, I. ; Mizutani, K. ; Kasahara, K. ; Yuda, T. ; Shibata, M. ; Shirai, T. ; Tateyama, N. ; Torii, Shoji ; Sugimoto, H. ; Taira, K. / Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala. In: Il Nuovo Cimento C. 1987 ; Vol. 10, No. 1. pp. 43-60.
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T1 - Primary cosmic-ray composition in the energy range of 1014 eV to 1016 eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala

AU - Ren, J. R.

AU - Kuang, H. H.

AU - Huo, A. X.

AU - Lu, S. L.

AU - Su, S.

AU - Wang, Y. X.

AU - Wang, C. R.

AU - He, M.

AU - Zhang, N. J.

AU - Cao, P. Y.

AU - Li, J. Y.

AU - Wang, S. Z.

AU - Bai, G. Z.

AU - Liu, Z. H.

AU - Li, G. J.

AU - Gang, G. X.

AU - Zhou, W. D.

AU - He, R. D.

AU - Amenomori, M.

AU - Nanjo, H.

AU - Hotta, N.

AU - Ohta, I.

AU - Mizutani, K.

AU - Kasahara, K.

AU - Yuda, T.

AU - Shibata, M.

AU - Shirai, T.

AU - Tateyama, N.

AU - Torii, Shoji

AU - Sugimoto, H.

AU - Taira, K.

PY - 1987/1

Y1 - 1987/1

N2 - We report on the results of the measurements of energy spectra of atmospheric cosmic rays in the energy around 10 TeV measured with emulsion chambers at Mt. Kanbala (5500 m above sea-level, atmospheric depth 520 g/cm2). The power indices of the integral spectra take the values of 2.00±0.08 for gamma-rays and 1.90±0.10 for hadrons, in the energy range from 5 TeV to 20 TeV. Their intensities are compatible with those expected from the primary cosmic rays containing fewer protons than in the lower energy region. The energy spectrum of family events is also discussed with reference to the composition of primary cosmic rays. It is concluded that the portion of protons in the primary cosmic rays gradually decreases in the energy range from 1013 eV to 1015 eV.

AB - We report on the results of the measurements of energy spectra of atmospheric cosmic rays in the energy around 10 TeV measured with emulsion chambers at Mt. Kanbala (5500 m above sea-level, atmospheric depth 520 g/cm2). The power indices of the integral spectra take the values of 2.00±0.08 for gamma-rays and 1.90±0.10 for hadrons, in the energy range from 5 TeV to 20 TeV. Their intensities are compatible with those expected from the primary cosmic rays containing fewer protons than in the lower energy region. The energy spectrum of family events is also discussed with reference to the composition of primary cosmic rays. It is concluded that the portion of protons in the primary cosmic rays gradually decreases in the energy range from 1013 eV to 1015 eV.

KW - Cosmic rays

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