Ultraheavy cosmic rays

Details Ultraheavy cosmic rays Ultraheavy cosmic rays

May 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975pht....28e..23i&link_type=abstract

Physics Today, vol. 28, May 1975, p. 23-27, 29-31.

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Abundance, Heavy Nuclei, High Energy Interactions, Primary Cosmic Rays, Balloon Sounding, Nuclear Fusion, Nuclides, Particle Acceleration, Particle Tracks, Satellite Observation, Skylab Program

Scientific paper

Ultraheavy cosmic rays consist of nuclei with an atomic number over thirty. The astrophysical significance of these nuclei as related to the various physical processes which have influenced their composition is considered, giving attention to the propagation of the particles through the interstellar medium, their acceleration in some source region, and their synthesis from lighter elements. Processes involved in the nucleosynthesis of ultraheavy elements include the s process, the r process, and the p process. The r process takes place on time scales of a few seconds in explosive events, presumably supernovae. The s process occurs probably in stars which are not exploding. Experimental results obtained in ultraheavy cosmic-ray experiments are discussed, giving attention to balloon-borne experiments and Skylab data.

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