A measurement of the cosmic-ray primary composition between 3 X 10 to the 13th and 3 X 10 to the 15th eV using underground muons

Details A measurement of the cosmic-ray primary composition between 3 X 10 to the 13th and 3 X 10 to the 15th eV using underground muons A measurement of the cosmic-ray primary composition between 3 X 10 to the 13th and 3 X 10 to the 15th eV using underground muons

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...358..637c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 358, Aug. 1, 1990, p. 637-643.

Mathematics

Probability

13

Abundance, Energy Spectra, Heavy Nuclei, Hodoscopes, Muons, Primary Cosmic Rays, Energetic Particles, Laboratory Equipment, Radiation Spectra, Scintillation Counters

Scientific paper

The multiplicities of high-energy muons (E(mu) greater than 2.6 TeV) detected deep underground by the Homestake liquid scintillation hodoscope are examined for sensitivity to the cosmic-ray primary composition in the energy range from 3 x 10 to the 13th to 3 x 10 to the 15th eV. Using a two-component (proton and iron) energy-independent composition model, it is found that the best primary composition model contains 83 + or - 13 percent protons and 17 percent iron. Using an energy-dependent five-component model, it is found that the multiple muon rates are in good agreement (67.4 chi sq probability) with a proton-dominated primary composition, as suggested by Fichtel and Linsley (1986). An iron-enriched primary composition does not provide a good fit to the experimental data (0.38 percent chi sq probability).

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