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Isotopes of Cosmic Ray Elements from Neon to Nickel

Published online by Cambridge University Press:  14 August 2015

C. J. Waddington ,
P. S. Freier ,
R. K. Fickle  and
N. R. Brewster
C. J. Waddington
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota, U.S.A.
P. S. Freier
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota, U.S.A.
R. K. Fickle
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota, U.S.A.
N. R. Brewster
Affiliation:
School of Physics and Astronomy, University of Minnesota, Minneapolis, Minnesota, U.S.A.

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We are reporting here on the results obtained from a balloon exposure of a cosmic ray detector flown in 1977. This detector, described elsewhere, Gilman and Waddington (1975), Young (1979), measures elemental charge from scintillation and Cherenkov signals and mass from Cherenkov and total energy determined from a measure of residual range in nuclear emulsion. The charge resolution obtained ranged from 0.19 to 0.21 charge units between neon and nickel. This resolution was sufficient to ensure that all but a few percent of the nuclei were correctly identified, even for those elements of low abundance that have neighbors with high abundances, such as Cl or Al. The mass resolution obtained for those nuclei that stopped in the emulsions ranged from 0.40 to 0.70 amu for A between 20 and 60 amu. This was not adequate to uniquely resolve neighboring mass peaks in many cases, but was adequate to draw a number of conclusions regarding many of the more abundant elements.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 94: Origin of Cosmic Rays , 1981 , pp. 33 - 34
Copyright
Copyright © Reidel 1981 

References

Gilman, C.M., and Waddington, C.J.: 1975, Proc. Munich Conf. 9, 3166.Google Scholar
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Mewaldt, R.A., Spalding, J.D., Stone, E.D., and Vogt, R.E.: 1980, Ap. J. Lett. 236, L121.CrossRefGoogle Scholar
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