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On the Detection of Heavy Primaries above 1014 EV

Published online by Cambridge University Press:  14 August 2015

T. K. Gaisser ,
Todor Stanev ,
Phyllis Freier  and
C. Jake Waddington
T. K. Gaisser
Affiliation:
Bartol Research Foundation of The Franklin Institute, University of Delaware, Newark, Delaware 19711
Todor Stanev
Affiliation:
Bartol Research Foundation of The Franklin Institute, University of Delaware, Newark, Delaware 19711
Phyllis Freier
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455
C. Jake Waddington
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota 55455

Extract

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Knowledge of the chemical composition is fundamental to understanding the origin, acceleration and propagation of cosmic rays. At energies much above 1014 eV, however, the detection of single primary cosmic rays is at present impossible because of their low flux, and the only source of information is from the cascades initiated by energetic primary particles in the atmosphere–the extensive air showers (EAS). A similar situation exists for the study of hadronic interactions above 1015 eV. A recent EAS experiment (Goodman et al., 1979) suggests the possibility that the spectrum becomes increasingly rich in heavy nuclei as the total energy per nucleus approaches 1015 eV. Above that energy the overall spectrum steepens and the question of composition is almost completely open.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 94: Origin of Cosmic Rays , 1981 , pp. 71 - 72
Copyright
Copyright © Reidel 1981 

References

Cassiday, G. L., et al.: 1978, Cosmic Rays and Particle Physics-1978 (Proc. Bartol Conf., ed. Gaisser, T. K.) AIP Conf. Proc. #49, p. 417.Google Scholar
Dixon, H. E., Turver, K. E., and Waddington, C. J.: 1974, Proc. Roy. Soc. A339, 157.Google Scholar
Goodman, J. et al.: 1979, Phys. Rev. Letters 42, 854.CrossRefGoogle Scholar
Jones, W. V., et al.: 1980, Bull. Am. Phys. Soc. 25, 546. See also Dake, S. et al.: 1979, Proc. 16th Int. Cosmic Ray Conf. (Kyoto) 6, 330.Google Scholar
Khristiansen, G. B.: 1979, Proc. 16th Int. Cosmic Ray Conf. (Kyoto) 14, 360 and references therein.Google Scholar
Orford, K., and Turver, K. E.: 1976, Nature 264, 727; see also Hammond, R. T., et al., N.C. 1c, 315 (1978).CrossRefGoogle Scholar
Tomaszewski, A. and Wdowczyk, J.: 1975, Proc. 14th Int. Cosmic Ray Conf. (Munich) 8, 2899.Google Scholar