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Title:
Energy spectra of cosmic-ray nuclei to above 100 GeV per nucleon
Authors:
Simon, M.; Spiegelhauer, H.; Schmidt, W. K. H.; Siohan, F.; Ormes, J. F.; Balasubrahmanyan, V. K.; Arens, J. F.
Affiliation:
AA(Max-Planck-Institut für extraterrestrische Physik, Garching bei München, Germany), AB(Max-Planck-Institut für extraterrestrische Physik, Garching bei München, Germany), AC(Max-Planck-Institut für extraterrestrische Physik, Garching bei München, Germany), AD(NASA, Goddard Space Flight Center, Greenbelt, Md.), AE(NASA, Goddard Space Flight Center, Greenbelt, Md.), AF(NASA, Goddard Space Flight Center, Greenbelt, Md.), AG(NASA, Goddard Space Flight Center, Greenbelt, Md.)
Publication:
Astrophysical Journal, Part 1, vol. 239, July 15, 1980, p. 712-724. Bundesministerium für Forschung und Technologie (ApJ Homepage)
Publication Date:
07/1980
Category:
Space Radiation
Origin:
STI
NASA/STI Keywords:
Cosmic Rays, Energy Spectra, Nuclei (Nuclear Physics), Backscattering, Balloon Sounding, Balloon-Borne Instruments, Cerenkov Counters, Energy Distribution, Monte Carlo Method
DOI:
10.1086/158157
Bibliographic Code:
1980ApJ...239..712S

Abstract

Energy spectra of cosmic-ray nuclei boron to iron have been measured from 2 GeV per nucleon to beyond 100 GeV per nucleon. The data were obtained using an ionization calorimeter flown on a balloon from Palestine, Texas. The 3450 kg payload floated at 7 g/sq cm for almost 24 hours. The results are in excellent agreement with those of other workers where overlaps exist. The spectra are not consistent with single power laws, and demonstrate the power of using a single technique sensitive over a large dynamic range. The data are consistent with the leaky box model of cosmic-ray propagation. The boron data indicate that the cosmic-ray escape length decreases with increasing energy as E to the -(0.4 + or - 0.1) up to 100 GeV per nucleon. Secondary nuclei from iron are also consistent with this dependence. Predicted changes in the energy dependence of the ratios of primary nuclei O/C and (Fe + Ni)/(C + O) are also observed.

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