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. Nanjo; N. Hotta; I. Ohta; K. Mizutani; K. Kasahara; T. Yuda; M. Shibata; T. Shirai; N. Tateyama; Shoji Torii; H. Sugimoto; K. Taira

doi:10.1007/BF02508696

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 › peer-review

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 language	English
Pages (from-to)	43-60
Number of pages	18
Journal	Il Nuovo Cimento C
Volume	10
Issue number	1
DOIs	https://doi.org/10.1007/BF02508696
Publication status	Published - 1987 Jan
Externally published	Yes

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)

Access to Document

10.1007/BF02508696

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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., ... 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, 10(1), 43-60. https://doi.org/10.1007/BF02508696

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 › peer-review

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, 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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title = "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",

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.",

keywords = "Cosmic rays",

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

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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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