Study of mass composition and energy spectrum of primary cosmic radiation by the imaging atmospheric Cherenkov technique

Details Study of mass composition and energy spectrum of primary cosmic radiation by the imaging atmospheric Cherenkov technique Study of mass composition and energy spectrum of primary cosmic radiation by the imaging atmospheric Cherenkov technique

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jphg...24..653p&link_type=abstract

Journal of Physics G: Nuclear and Particle Physics, Volume 24, Issue 3, pp. 653-672 (1998).

Physics

7

Scientific paper

Imaging atmospheric Cherenkov telescopes (IACT) have proven to be, up to now, the most effective instruments for the observation of primary TeV 0954-3899/24/3/015/img11-radiation from astrophysical objects. The high detection rate as well as the capability of accurate reconstruction of air-shower parameters by the IACT technique also allow the use of the imaging technique for the study of the energy spectrum and mass composition of cosmic rays. In this paper we discuss the potential of this technique for the separation of different components of cosmic rays in the energy region 1-0954-3899/24/3/015/img12. We show that the imaging technique allows adequate separation of showers produced by protons from the contributions of all other nuclei, including 0954-3899/24/3/015/img13-particles, and thus allows a measurement of the energy spectrum of the proton component at TeV energies. Such measurements can currently be performed by operating single IACTs designed originally for 0954-3899/24/3/015/img11-ray astronomical purposes. The effective separation of different nucleus groups of the cosmic radiation is a more difficult problem. It benefits from the stereoscopic reconstruction of the shower development in the Earth's atmosphere. Our calculations show that simultaneous detection of air showers by two IACTs located at a distance of about 100 m from each other allows an effective separation of the proton, 0954-3899/24/3/015/img13-particle, medium (O), heavy (Si), and very heavy (Fe) groups of cosmic-ray nuclei.

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