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Energy spectra of cosmic ray nuclei: 4≤Z≤26 and 0.3≤E≤2 GeV amu−1

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Abstract

Energy spectra of cosmic ray nuclei in the charge range 5≤Z≤26 have been derived from the response of an acrylic plastic Čerenkov detector. Data were obtained using a balloon-borne detector and cover the energy range 320≲E≲2200 MeV amu−1. Spectra are derived from a formal deconvolution using the method of Lezniak (1975). Relative spectra of different elements are compared by observing the charge ratios. Secondary-primary ratios are observed to decrease with increasing energy, consistent with the effect previously observed at higher energy. Primary-to-primary ratios are constant for 6≤Z≤10 and 14≤Z≤26 but vary for 10≤Z≤14. This data is found to be consistent with existing data, where comparable, and lends strong support to the idea of two separate source populations contributing to the cosmic ray composition.

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Authors and Affiliations

  1. NASA/Goddard Space Flight Center, Greenbelt, Maryland, USA

    R. C. Maehl (Work performed as NAS/NRC Resident Research Associate), J. F. Ormes, A. J. Fisher & F. A. Hagen

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  1. R. C. Maehl
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  2. J. F. Ormes
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  3. A. J. Fisher
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  4. F. A. Hagen
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Work supported by University of Maryland Grant NGR 21-002-316.

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Maehl, R.C., Ormes, J.F., Fisher, A.J. et al. Energy spectra of cosmic ray nuclei: 4≤Z≤26 and 0.3≤E≤2 GeV amu−1 . Astrophys Space Sci 47, 163–184 (1977). https://doi.org/10.1007/BF00651365

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  • DOI: https://doi.org/10.1007/BF00651365

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