Cosmic ray chemical composition estimated between 2x10^14 eV and 2x10^16 eV using muon size fluctuations

Details Cosmic ray chemical composition estimated between 2x10^14 eV and 2x10^16 eV using muon size fluctuations Cosmic ray chemical composition estimated between 2x10^14 eV and 2x10^16 eV using muon size fluctuations

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aph.....3..125m&link_type=abstract

ASTROPARTICLE PHYSICS, Volume 3, Issue 2, p. 125-136.

Physics

4

Scientific paper

Accurate measurement of the total number of muons in an air shower is important for estimating the cosmic ray chemical composition. In order to translate this view into action, we have constructed an air shower array at Ohya. Many large muon detectors have been deployed in the stone mine and the total area amounts to about 400 m^2. At the ground surface, scintillation counters have been deployed for determining the shower size and arrival direction of an air shower. From the data obtained, we estimated the cosmic ray chemical composition between 2x10^14 eV and 2x10^16 eV, which includes the well known spectrum's ``knee''. As a method of estimation, we took the muon size fluctuation. The estimated rate of protons becomes relatively low, and that of helium nuclei increases, above an energy of 2x10^15 eV. Also, the fraction of very heavy nuclei such as iron increases above this energy.

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