The propagation of ultraheavy cosmic ray nuclei

Details The propagation of ultraheavy cosmic ray nuclei The propagation of ultraheavy cosmic ray nuclei

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...264..324b&link_type=abstract

Astrophysical Journal, Part 1, vol. 264, Jan. 1, 1983, p. 324-336.

Astronomy and Astrophysics

Astrophysics

22

Abundance, Astronomical Models, Cosmic Rays, Heavy Nuclei, Particle Acceleration, Barium, Cadmium, Lead (Metal), Particle Trajectories, Platinum, Ruthenium, Solar System, Tin

Scientific paper

The propagation of ultraheavy cosmic ray nuclei (Z greater than 30) has been studied using a model based on the leaky-box formalism. This model has been used to examine the possible composition of the source, the path length distribution, and the mean escape length of the confinement region. Various abundance ratios have been found that have a sensitive dependence on one or more of these factors. Comparison of the theoretical values of these ratios with published data suggests that the source composition is similar to that of solar system matter, but that in the Pt-Pb region, enrichment in material produced by the r-process cannot be ruled out. Data for the secondary-to-primary ratio (Ru-44 - Cd-48)/(Sn-50 - Ba-56) show the presence of significantly more secondaries than are predicted, even when a truncated path length distribution is used in the model.

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