``Quasidirect'' observations of cosmic-ray primaries in the energy region 1012-1014 eV

Details ``Quasidirect'' observations of cosmic-ray primaries in the energy region 1012-1014 eV ``Quasidirect'' observations of cosmic-ray primaries in the energy region 1012-1014 eV

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phrvd..40..729k&link_type=abstract

Physical Review D (Particles and Fields), Volume 40, Issue 3, 1 August 1989, pp.729-753

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Scientific paper

We have exposed an emulsion chamber at a level of 32.8 g/cm2 for ~30 h, and detected ~800 showers on x-ray films (Fuji No. 200 type). Among these, ~200 primaries (Σ Eγ>=2 TeV, θ<75°) were identified by tracing back through successive plates of nuclear emulsion. On the basis of these primaries, we obtain Ip(>=E0)=1.02×10-5 [E0/(1 TeV)]-1.82+/-0.13 (cm2 sec sr)-1 in the region 5<~E0<~100 TeV for proton primaries, and Iα(>=E0) =6.50×10-7[E0/(1 TeV/nucleon)]-1.75+/-0.15 (cm2 sec sr)-1 in the region 3<~E0<~10 TeV/nucleon for α primaries. We observed also many atmospheric secondary γ rays, which cover the energy region 2-80 TeV. The γ-ray spectrum is a rather smooth continuation of that obtained by Nishimura et al. in the region 0.2-2 TeV. The higher-energy part of our flux, however, cannot be reproduced by the atmospheric nuclear interaction of the primary protons and α particles alone, indicating that, for energies >~1014 eV/nucleus, the contribution of heavier primaries becomes significant, and that the latter flux may very well become comparable with the proton flux somewhere between 1014 and 1015 eV/nucleus. This indication is consistent with the iron flux obtained directly by the present experiment, though poor statistics preclude a conclusive result.

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