Abundances and spectra for cosmic-ray nuclei from lithium to iron for 2 to 150 GeV per nucleon

Details Abundances and spectra for cosmic-ray nuclei from lithium to iron for 2 to 150 GeV per nucleon Abundances and spectra for cosmic-ray nuclei from lithium to iron for 2 to 150 GeV per nucleon

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...226.1147o&link_type=abstract

Astrophysical Journal, Part 1, vol. 226, Dec. 15, 1978, p. 1147-1161. Research supported by the U.S. Department of Energy;

Astronomy and Astrophysics

Astrophysics

55

Abundance, Energy Spectra, Particle Energy, Primary Cosmic Rays, Astronomical Models, Balloon-Borne Instruments, Data Reduction, Electric Charge, Instrument Errors, Propagation, Superconducting Magnets

Scientific paper

Measurements of primary cosmic-ray composition and energy spectra made with a balloon-borne superconducting magnetic spectrometer are described. Results for both 6.7 g/sq cm equivalent vertical atmospheric depth and the top of the atmosphere are presented for the absolute and relative integral abundances, the differential energy spectra, and the spectral indices for cosmic-ray nuclei from Li to Fe and energies of 2 to 50 GeV/n. It is found that propagation effects can explain essentially all the elemental abundances, that the abundances of Li, Be, and B for rigidities below 10 GV/c are consistent with an energy-independent mean interstellar path length of 4.5 + or - 0.5 g/sq cm for the 'leaky box' propagation model, that the abundances of all elements above 10 GV/c are consistent with a path length that decreases as the inverse n-th power of rigidity, and that n equals 0.6 (+0.4, -0.3) for the simplest assumptions made in fitting the source spectra.

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