Composition of primary cosmic rays at energies 10(15) to approximately 10(16) eV

Details Composition of primary cosmic rays at energies 10(15) to approximately 10(16) eV Composition of primary cosmic rays at energies 10(15) to approximately 10(16) eV

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....2..206a&link_type=abstract

In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 2 p 206-209 (SEE N85-34006 22-93)

Physics

Cosmic Ray Showers, Energy Distribution, Energy Spectra, Flux Density, Particle Density (Concentration), Protons, Electron Distribution, Monte Carlo Method, Particle Emission, Secondary Cosmic Rays

Scientific paper

The sigma epsilon gamma spectrum in 1 approx. 5 x 1000 TV observed at Mt. Fuji suggests that the flux of primary protons 10 to the 15 approx 10th eV is lower by a factor of 2 approx. 3 than a simple extrapolation from lower energies; the integral proton spectrum tends to be steeper than around to the power V and the spectral index tends to be steeper than Epsilon to the -17th power around 10 to the 14th power eV and the spectral index becomes approx. 2.0 around 10 to the 15th power eV. If the total flux of primary particles has no steepening up to approx 10 to the 15th power eV, than the fraction of primary protons to the total flux should be approx 20% in contrast to approx 45% at lower energies.

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