Elemental abundance of high energy cosmic rays
K. Asakimori, Kobe Women's University
T. H. Burnett, University of Washington
M. L. Cherry, Louisiana State University
K. Chevli, The University of Alabama in Huntsville
M. J. Christl, NASA Marshall Space Flight Center
S. Dake, Kobe University
J. H. Derrickson, NASA Marshall Space Flight Center
W. F. Fountain, NASA Marshall Space Flight Center
M. Fuki, Kochi University
J. C. Gregory, The University of Alabama in Huntsville
R. Holynski, Henryk Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences
J. Iwai, University of Washington
A. Iyono, Okayama University of Science
W. V. Jones, Louisiana State University
A. Jurak, Henryk Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences
M. Kobayashi, High Energy Accelerator Research Organization, Tsukuba
J. J. Lord, University of Washington
O. Miyamura, Hiroshima University
H. Oda, Kobe University
T. Ogata, The University of Tokyo
E. D. Olson, University of Washington
T. A. Parnell, NASA Marshall Space Flight Center
F. E. Roberts, NASA Marshall Space Flight Center
T. Shiina, The University of Alabama in Huntsville
S. C. Strausz, University of Washington
Y. Takahashi, The University of Alabama in Huntsville
T. Tominaga, The University of Alabama in Huntsville
S. Toyoda, The University of Tokyo
J. W. Watts, NASA Marshall Space Flight Center
Wefel, Louisiana State University
B. Wilczynka, Henryk Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences
H. Wilczynski, Henryk Niewodniczanski Institute of Nuclear Physics of the Polish Academy of Sciences
R. J. Wilkes, University of Washington
Abstract
Very high energy spectra of cosmic ray nuclei from the JACEE balloon experiments are presented. From a total of 12 balloon flights with an exposure factor of about 580 m2hour the energy spectra of nuclei have been obtained in the energy range from several TeV to 1,000 TeV. Proton energy spectrum, extending to several hundred TeV, can be a single-power law. Helium shows a single power law spectrum in the energy range from 2 TeV/n to 200 TeV/n. Other nuclei up to Fe indicated harder spectral indices compared with those of protons and helium. The composition at around 500 TeV is 16 ± 5%: 29 ± 5%: 35 ± 5%: 9 ± 3%: 11 ± 4%, for the abundance of p : He : C ∼ O : Ne ∼ S : Z ≥ 18.
