Method for studying the chemical composition of the primary cosmic radiation at and above 10 to the 17th eV

Details Method for studying the chemical composition of the primary cosmic radiation at and above 10 to the 17th eV Method for studying the chemical composition of the primary cosmic radiation at and above 10 to the 17th eV

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981zhpmr..33..236a&link_type=abstract

(ZHETF Pis'ma v Redaktsiiu, vol. 33, Feb. 20, 1981, p. 236-239.) JETP Letters, vol. 33, Feb. 20, 1981, p. 225-227. Translation.

Computer Science

1

Chemical Composition, Energetic Particles, Muons, Primary Cosmic Rays, Radiation Counters, Cerenkov Radiation, Cosmic Ray Showers, High Energy Interactions, Nucleon-Nucleon Interactions

Scientific paper

A new method is proposed for studying the chemical composition of primary cosmic rays, based on measurements of not only the primary energy for extensive air showers (EAS) and the number of muons in it, but also the position of the EAS maximum. A procedure for determining the position of this maximum from the shape of the Cerenkov-radiation pulse, proposed by Fomin and Khristiansen (1971), is adopted. It is shown that fixing the primary energy for the EAS as well as the position of the maximum reduces the relative fluctuations in the number of muons, while having essentially no effect on the exponent 'a'. The exponent 'a' in the expression Nmu approximately = E0 exponent 'a', gives the number of muons in the EAS as a function of the primary energy. Fixing these parameters makes it easier to resolve different groups of nuclei.

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