Primary cosmic-ray composition in the energy range of 10 to the 14th eV to 10 to the 16th eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala

Details Primary cosmic-ray composition in the energy range of 10 to the 14th eV to 10 to the 16th eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala Primary cosmic-ray composition in the energy range of 10 to the 14th eV to 10 to the 16th eV and high-energy atmospheric cosmic rays observed with emulsion chambers at Mt. Kanbala

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ncimc..10...43r&link_type=abstract

Nuovo Cimento C, Serie 1 (ISSN 0390-5551), vol. 10 C, Jan.-Feb. 1987, p. 43-60. Research supported by the Chinese Academy of Sci

Computer Science

8

Cosmic Ray Showers, Energy Spectra, Gamma Rays, Hadrons, Nuclear Emulsions, Primary Cosmic Rays, Protons, Computerized Simulation, Monte Carlo Method, Mountains, Muons

Scientific paper

The results of measurements of energy spectra of atmospheric cosmic rays at around 10 TeV with emulsion chambers at Mt. Kanbala (5500 m above sea-level, atmospheric depth 520 g/sq cm) are reported. The power indices of the integral spectra take the values of 2.00 + or - 0.08 for gamma rays and 1.90 + or - 0.10 for hadrons, in the energy range 5-20 TeV. Their intensities ae compatible with those expected from 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 10 to 1000 TeV.

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