Energy spectrum of surviving primary protons with energies(3÷30) TeV at5200 m a.s.l. and the cross-section for proton-air-nucleus collisions

We consider a relationship between the difference in spectral indices of the spectra of single hadrons and all hadrons ( β sngl -β h ) and the difference in the indices of the spectra of galactic cosmic ray (GCR) protons and nuclei. It is demonstrated that at the mountain level the ratio ( β p -β Z )/( β sngl -β h ) is always larger than unity, if ( β sngl -β h ) > 0.1. From the experimental value β sngl -β h = 0.4 ± 0.05 we derive that, in the vicinity of E = 10 TeV, β p -β Z ≥ 0.49 ± 0.06 , i.e., β p ≥ 3.09 ± 0.06 .

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The time structure of atmospheric Cerenkov light in extensive air showers

Böhm

Bosia

Navarra

et al. 1977

J. Phys. A: Math. Gen.

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Energy spectrum of surviving primary protons with energies(3÷30) TeV at5200 m a.s.l. and the cross-section for proton-air-nucleus collisions

Cited by 6 publications

References 10 publications

On the apparent break of scaling features in high-energy cosmic-ray components in the atmosphere

On the apparent break of scaling features in high-energy cosmic-ray components in the atmosphere

A new method of determining the spectral index for protons in the energy range about 1013 eV

The time structure of atmospheric Cerenkov light in extensive air showers

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