Abundance of primary protons at (1-3)×1015 eV inferred from a simulation of extensive air showers with γ-ray families

Details Abundance of primary protons at (1-3)×1015 eV inferred from a simulation of extensive air showers with γ-ray families Abundance of primary protons at (1-3)×1015 eV inferred from a simulation of extensive air showers with γ-ray families

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phrvd..39.1275s&link_type=abstract

Physical Review D (Particles and Fields), Volume 39, Issue 5, 1 March 1989, pp.1275-1282

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Scientific paper

A Monte Carlo simulation of extensive air showers (EAS's) was done under a particle-interaction model and was compared with the EAS's accompanied by γ-ray and hadronic families with total energy JEγ,H greater than 10 TeV obtained in the Mt. Norikura experiment (2780 m above sea level). The strong correlation between the shower size Ne of EAS's with family and the primary energy, E0, was obtained from the simulation as E0/Ne=(2.0+2.7-0.7) GeV with 95% width. The flux of the EAS's with family is sensitive to the chemical composition, especially to the fraction of protons in the primary cosmic-ray particles. The fraction of protons is inferred to be (20+/-6)% and (23+/-9)%, with one standard deviation (1σ), at energy (1.4+1.9-0.5)×1015 eV and (2.8+3.8-1.0)×1015 eV with 95% confidence interval, respectively, under the assumption of increasing cross section σp-air~E0.055 and approximate Feynman scaling in the fragmentation region. These values are in agreement with the values obtained from other mountain emulsion-chamber experiments within 2σ. The proton fraction thus obtained, around 20%, is much less than the normal abundance (~40%) expected from direct observations at lower energies around 1012 eV.

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